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701 | Discovery of Optical Transient TSS J004150.4+404222 in M31 | R. Quimby, F. Castro, M. Sellers, P. Hoeflich, E. L. Robinson, J. C. Wheeler (University of Texas), and A. Shafter (SDSU) | We report the discovery of an optical transient near M31 using unfiltered CCD images taken on 2006 Jan 5.08 UT (about 17.2 mag) and Jan 9.08 (about 16.9 mag) using the 0.45m ROTSE-IIIb telescope at the McDonald Observatory. The object is located at RA = 00h41m50.42s DEC = +40o42'22.5" (J2000), which is 10' 7.7" west and 33' 46.0" south of the core of M31. TSS J004150.4+404222 was not detected in ROTSE-IIIb data from 2005 Dec 31.08 UT (limiting mag about 17.8). The transient increased in brightness irregularly for 10 days, reaching about 15.9 mag on Jan 14.08, and then faded to about 17.0 mag on Jan 19.09. The light curve suggests the object may be a nova or a bright, unusual variable star such as a Luminous Blue Variable. | 2006-01-21 02:22:00 | optical,cataclysmic variable,nova,star,transient,variables | 2006-01-21 | 02:22:00 | 731 | [
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] | 700 |
702 | Swift/XRT localization of XRT J1701-462 | J. A. Kennea (PSU), F. Marshall(GSFC), D. Steeghs (CFA), C. Markwardt (GSFC/UMD), D. N. Burrows (PSU), M. Torres (CfA), J. Miller (U. Michigan), S. Hunsberger (PSU), J. Nousek (PSU) and N. Gehrels (GSFC) | At 19:16 UT on January 20th, 2005, Swift began a target of opportunity observation of the RXTE discovered transient XTE J1701-462 (ATEL#696, #700). The Swift/XRT on-board centroiding algorithm located a bright, previously uncatalogued point source at the following coordinates: RA(J2000): 17:00:57.2 Dec(J2000): -46:11:16.8 with a error radius of 5.8 arcseconds (90% containment). This position lies 71 arcseconds from the refined XTE position reported by Markwardt et al. (2006, ATEL #700). The measured flux was 1.4 x 10^-8 erg/s/cm^2 (0.2-10 keV), uncorrected for absorption and assuming a Crab-like spectrum. Further observations of this target by Swift are planned. | 2006-01-21 03:35:00 | x-ray,transient | 2006-01-21 | 03:35:00 | 670 | [
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] | 701 |
703 | RXTE Pointed Observations of XTE J1701-462 | T. E. Strohmayer, J. H. Swank (NASA/GSFC), E. H. Morgan (MIT), C. B. Markwardt (NASA/GSFC &UMD), N. Shaposhnikov (NASA/GSFC & USRA) | The RXTE PCA and HEXTE observed the new transient XTE J1701-462 (Remillard et al, ATEL #696) first on 19 Jan 2006 at 18:00 UT for 3800 seconds. Observations on 20 Jan (Markwardt & Swank, ATEL #700) included several pointed observations. The fluxes on 19 Jan were 1.7e-8 and 2.8e-9 ergs cm^-2 s^-1 in the 2-10 keV and 10-40 keV bands respectively. On 20 Jan they rose as high as 1.9e-8 and 3.3e-9, respectively, decreased to a third of that and started to recover.
It is not obvious what it is. The source does not fit canonical spectral or timing characteristics for a pulsar, an LMXB, or a black hole. The simplest approximate descriptions of the spectra use absorbed bremsstrahlung with kT ~2.5-4 keV, the kT correlated to the luminosity. The PCA sees a column density of 2-3 x 10^22 cm^-2, depending on the model. HEXTE detected the source and there may be a power law extension of the spectra. There is varying rms variability. Power spectra evolved over the day of observations, with noise present below 0.1 Hz and QPO of a few percent sometimes very significant near 6 and 55 Hz. In the last observation there were flux swings of 30% with time scales of several minutes.
Additional RXTE observations are planned. | 2006-01-21 10:02:00 | x-ray,binary,black hole,neutron star,pulsar,star,transient,request for observations | 2006-01-21 | 10:02:00 | 1,220 | [
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] | 702 |
704 | Swift X-ray Spectrum and V-band Upper Limit for XTE J1701-462 | J. A. Kennea (PSU), F. E. Marshall(GSFC), D. Steeghs (CFA), C. Markwardt (GSFC/UMD), D. N. Burrows (PSU), M. Torres (CfA), J. Miller, S. Hunsberger (PSU), J. Nousek (PSU) and N. Gehrels (GSFC) | We have analyzed the 500s of Swift/XRT data on the newly discovered X-ray transient XTE J1701-462 (ATEL #696, #700, #702). The source was bright, with a count rate approximately 230 counts/s, which does not vary significantly during the observation. The spectrum is well fit by an absorbed power-law model with NH = (2.7 ± 0.1) x 1022 cm-2 and a photon index of 1.9 ± 0.1. The expected value for galactic NH in this direction is 9 x 1021 cm-2. The X-ray flux is 1.8 x 10-8 erg/s/cm2 (0.5 - 10 keV), or 3.4 x 10-8 erg/s/cm2 (0.5 - 10 keV) corrected for absorption. The X-ray luminosity is ~3 x 1038 erg/s for an assumed distance of 8.5 kpc.
The source is not detected in a 671-second observation with Swift/UVOT starting at 19:19:59 UT on 20 Jan. The 3-sigma upper limit is V=19.3 uncorrected for the expected visual extinction of 12.7 mag.
Additional Swift observations are planned. | 2006-01-21 12:28:00 | optical,x-ray,binary,black hole,neutron star,star,transient | 2006-01-21 | 12:28:00 | 886 | [
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] | 703 |
705 | Discovery and Classification of Three Supernovae | The Nearby Supernova Factory: G. Aldering, S. Bailey, S. Bongard, D. Kocevski, B. C. Lee, S. Loken, P. Nugent, S. Perlmutter, R. Scalzo, R. C. Thomas, L. Wang, B. A. Weaver (Lawrence Berkeley National Laboratory, Berkeley, CA), N. Blanc, Y. Copin, E. Gangler, L. Sauge, G. Smadja (Institut de Physique Nucleaire de Lyon), P. Antilogus, S. Gilles, R. Pain, R. Pereira (Laboratoire de Physique Nucleaire et de Haute Energies de Paris), E. Pecontal, G. Rigaudier (Centre de Recherche Astronomique de Lyon), R. Kessler (Kavli Institute for Cosmological Physics, Chicago, IL), C. Baltay, D. Rabinowitz, A. Bauer (Yale) | The Nearby Supernova Factory reports the discovery and classification of three supernovae in images obtained using the QUEST II camera on the Palomar Oschin 48-inch telescope as a part of the JPL Near-Earth Asteroid Tracking component of the Palomar Consortium. Discovery image dates and approximate magnitudes (calibrated to R) are listed in the table below. Spectra (range 320-1000 nm) of these objects obtained Jan. 18 UT with the Supernova Integral Field Spectrograph on the University of Hawaii 2.2-meter telescope were used for classification. | 2006-01-22 01:07:00 | infra-red,optical,ultra-violet,asteroid,supernovae | 2006-01-22 | 01:07:00 | 549 | [
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] | 704 |
706 | Optical Counterpart of J1701-462 | D. Maitra, C. Bailyn, J. Nelan (YALE), J. Espinoza (CTIO/SMARTS) | We obtained H-band images of the SWIFT error field of J1701-462 (ATel #702) using the SMARTS 1.3m telescope and ANDICAM instrument on Jan 21.3707 UT. We find a new object not present in the 2MASS catalogue. The H-band magnitude of the new source was 16.5 +- 0.1 in the Jan 21 data, as determined by comparison with nearby stars in the field with known 2MASS photometry. We find the coordinates of this new source to be: RA = 17:00:58.45 Dec = -46:11:08.6 with an error of approximately 0.5". A finding chart is available at: http://www.astro.yale.edu/maitra/J1701-462/ | 2006-01-22 13:04:00 | infra-red,optical,x-ray,binary,black hole,neutron star,star,transient | 2006-01-22 | 13:04:00 | 568 | [
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] | 705 |
707 | X-ray activity in GX 339-4 | N. Bezayiff and D. M. Smith (U. C. Santa Cruz) | Observations with the Rossi X-ray Timing Explorer (RXTE) show that the suspected black-hole binary GX 339-4 has become active after 8 months in quiescence. Three consecutive monitoring observations taken with the Proportional Counter Array (PCA) on 15 January (20:52 UT), 18 January (18:54 UT), and 21 January (07:38 UT) are all significantly above background, and show an increase with time in count rate from 1.0 to 3.8 to 5.8 counts/s/PCU. These rates are less than 1% of peak outburst levels, and it is not yet clear whether this represents a new outburst or variable low-level activity as was seen throughout 1996 and 1997 (see, e.g., Smith et al. 2002, ApJ 569, 362, Figure 4). The unabsorbed fluxes for these three observations rise from approximately 10^-12 to 10^-11 erg/cm2/s.
The spectra are shown in the figure linked below (white = Jan. 15, red = Jan. 18, green = Jan. 21). The two earlier spectra require a disk blackbody component in addition to a hard power law, while the latest is consistent with the canonical hard state, showing only a small improvement in the fit by the addition of a disk blackbody.
The iron line in the first observation is striking, and is fit with an equivalent width of (3.2 +/- 1.6) keV and center of (6.57 +/- 0.14) keV. The equivalent width declined to (790 +/- 460) eV by 18 January and (270 +/- 320) eV by 21 January. It is interesting that these data appear consistent with a simple power law being gradually added to the initial spectrum of 15 January.
Feng et al. (2001, ApJ 553, 394) reported that at very low flux, the iron line from GX 339-4 approached the He-like line energy of 6.7 keV and had a large equivalent width of up to 500 eV. The measurement of an equivalent width of over 3 keV, although not of high statistical significance, is the highest we have measured in any black hole system during our monitoring campaigns with the PCA, and suggests a continuation of the trend reported by Feng et al. We are exploring a pure reflection spectrum as a possible explanation of the 15 January data. No iron line is seen in the many observations we have made in quiescence, so Galactic diffuse emission is not responsible for this feature.
As always in what may be the early stages of a LMXRB transient outburst, multiwavelength observations are strongly encouraged.
Erratum: In ATEL #322, we reported that during the transition from the hard to soft state in last summer's outburst of GX 339-4, the observation made at 14h on 17 August, 2005 showed a soft energy spectrum but had an active power spectrum, with band-limited noise and a QPO, and therefore we described the system as being in the Very High State at that time. The power spectrum we reported as belonging to this date was an earlier one. The system was actually in the High/Soft state at this time, with little variability, as has been reported in a thorough paper on this outburst by Belloni et al. (astro-ph/0601031, accepted by MNRAS). | 2006-01-23 10:01:00 | x-ray,binary,black hole,transient,variables,request for observations | 2006-01-23 | 10:01:00 | 2,963 | [
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] | 706 |
708 | XTE J1701-462 seen by INTEGRAL | N. Produit (ISDC, Geneva), A. Bazzano (IASF, Roma), V. Schoenfelder (MPE, Garching), N.-J. Westergaard (DSRI, Copenhagen), B. McBreen (Univ. College, Dublin), R. Much (ESTEC, Noordwijk), W. Hermsen (SRON, Utrecht), S. Molkov (IKI, Moscow) | The newly discovered X-ray transient XTE J1701-462 (ATEL #696, #700, #702, #703, #704, #706) was in the field of view of the INTEGRAL instruments during a routine Galactic Plane Scan on 2006 Jan. 21 at 03:45 UT, during one pointing of 1850 sec in JEM-X and three pointings in IBIS. It was detected by the JEM-X instrument with a flux of 58+-6 counts/s in 3-10 keV (about 0.9 Crab) and 2.8+-0.5 counts/s in 10-20 keV (about 0.13 Crab). It was not detected in ISGRI, with an upper limit of 5 mCrabs above 20 keV. The INTEGRAL spectrum cannot be represented with a powerlaw. A thermal bremsstrahlung with kT = 3 keV fits the data. | 2006-01-24 00:18:00 | x-ray,transient | 2006-01-24 | 00:18:00 | 627 | [
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] | 707 |
709 | Probable Optical Counterpart of IGR J00234+6141 | J. P. Halpern (Columbia. U.), N. Mirabal (U. Michigan) | We report a probable identification of the weak hard X-ray source IGR J00234+6141 (den Hartog et al., ATel #394) with a star that has an optical spectrum of a cataclysmic variable. den Hartog et al. noted the presence of a ROSAT All-Sky Survey source 1RXS J002258.3+614111 located 3.15' from the INTEGRAL position and marginally consistent with it, given the estimated 3' error radius (90% confidence) of the latter. On two observing runs using the the MDM 2.4m telescope, we obtained low-resolution spectra of 14 bright stars within 3' of the INTEGRAL position, and another 10 stars within 1' of the ROSAT position. Only one of these stars shows emission lines. The discovery spectrum was obtained on 2006 January 24 UT. It shows four emission lines of the Balmer series, the strongest being H-alpha with E.W.=3.7 nm. He I 5876, He I 6678, and He I 7065 are also present. There is also a He II 4686 line of E.W. approximately 2/3 that of H-beta. These properties are typical of X-ray emitting cataclysmic variables. The magnitudes of the star in the USNO-B1.0 and 2MASS catalogs are B=18.01, R=16.34, I=15.63, J=15.12, H=15.05, K=14.77. Its location at R.A. = 00h 22m 57.63s, Decl. = +61o 41' 07.8" (J2000), only 6" from the ROSAT position, makes it a secure counterpart of the ROSAT source. The absence of any additional optical candidate among the examined stars closer to the INTEGRAL position argues that the INTEGRAL source is identical to the ROSAT source, although it doesn't prove it . | 2006-01-25 11:15:00 | optical,x-ray,cataclysmic variable,star,variables | 2006-01-25 | 11:15:00 | 1,494 | [
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] | 708 |
710 | XTE J1701-462: possible radio counterpart | Rob Fender (Southampton), Bob Sault (ATNF), Michael Dahlem (ATNF) | An observation of the field of the new X-ray transient XTE J1701-462 (ATEL #696, #702, #708) was performed with the Australia Telescope Compact Array on 2006 Jan 22. The observation was made simultaneously at 4.8 and 8.6 GHz over a period of approximately 75 minutes beginning 21:45 UT. A radio source is detected at the location (within uncertainties of order one arcsec) of the infrared counterpart reported by Maitra et al. (ATEL #706), with a flux density of approximately 0.5 mJy at 4.8 GHz. If associated with the X-ray transient, this radio emission is likely to be the signature of a relativistic ejection event. | 2006-01-25 18:19:00 | radio,x-ray,binary,black hole,neutron star,star,transient | 2006-01-25 | 18:19:00 | 620 | [
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] | 709 |
711 | Vela X-1 in a highly active state | I. Kreykenbohm (ISDC, Geneva & IAA, Tuebingen), R. Staubert (IAA, Tuebingen), A. von Kienlin (MPE, Garching), S. Martinez-Nunez (Valencia), M. Mas-Hesse (LAEFF, Madrid), C. Sanchez (ESAC, Madrid), G. G.C. Palumbo (Bologna University), R. A. Sunyaev (IKI, Moscow & MPA, Garching) | Recent routine INTEGRAL Galactic Plane Scan (GPS) observations including the Vela region have shown that Vela X-1 has entered a highly active state, similar to the December 2003 flaring state (Staubert et al., 2004, Conf. Proc. 5th Integral Workshop). During the GPS observations on 2006 January 16 and 2006 January 22, Vela X-1 was in the field of view of ISGRI for 9 ksec and 12 ksec, respectively. The averaged flux in both observations was approximately 0.7 Crab (20-40 keV). On top of the already high average flux level, flaring behavior with a flux increase by a factor of 3 was observed: in some pointings, the average flux was higher than 1 Crab with a maximum of almost 1.5 Crab (20-40 keV). More detailed analysis of the ISGRI lightcurve in the 20-40 keV band with a time resolution of 20 seconds showed that the source was strongly pulsating with a pulsed fraction around 75%. During the pulse maxima, count rates of more than 200 cts/sec were frequently observed, the peak count rate being 305 cts/sec which corresponds to more than 2.5 Crab. Above 40keV, the source was still strongly detected, but the average count rate was only 10% of the 20-40 keV rate and no flares were evident. Unfortunately the source was neither in the field of view of JEM-X nor the optical monitor OMC during both observations. Since the spectrometer SPI was annealing, also no high resolution spectral data are available. Follow-up observations are strongly encouraged. | 2006-01-26 22:54:00 | optical,x-ray,gamma ray,binary,neutron star,pulsar,star,request for observations | 2006-01-26 | 22:54:00 | 1,462 | [
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] | 710 |
712 | Near-Infra-Red Observations of XTE J1701-462 using SMARTS | D. Maitra, C. Bailyn (Yale) | We have been observing the putative near-infra-red counterpart of the newly discovered X-ray transient XTE J1701-462 (ATEL #696, #702, #706, #710), in I, J, H and K-bands, using the SMARTS 1.3m telescope and ANDICAM instrument since Jan 21. As of Jan 26.36 UT, the magnitudes of the source were: I=20.3(2) J=16.8(1) H=15.7(1) K=15.0(1) The lightcurves show significant variability (~0.8 mag in I-band and ~0.6 mag in H-band). The variability appears to be correlated among the bandpasses. Although this source is outside the XRT error box, it nevertheless shows characteristics appropriate for the counterpart of this X-ray source, in particular reddened colors and day-to-day variability. | 2006-01-27 03:42:00 | infra-red,x-ray,binary,black hole,neutron star,star,transient | 2006-01-27 | 03:42:00 | 689 | [
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] | 711 |
713 | SWIFT J1626.6-5156 is not a high mass X-ray binary | N. Rea (SRON Utrecht), V. Testa, G. L. Israel, A. Antonelli (INAF-OAR), P. Jonker (SRON Utrecht, CfA), T. Belloni, S. Campana (INAF-OAB), L. Stella (INAF-OAR) | on behalf of E. Molinari, G. Chincarini, F.M. Zerbi, S. Covino, G. Tosti, P. Conconi, G. Cutispoto, L. Nicastro, E. Palazzi, F. Vitali, F. D'Alessio, E. Meurs, P. Goldoni and the REMIR/ROSS collaboration
We report on infrared observations of the newly discovered transient X-ray pulsar SWIFT J1626.6-5156 (Palmer et al., ATEL #678, Markwardt & Swank, ATEL #679 and Campana et al., ATEL #688). The observations were performed in J, H and K filters every night from 2006 January 15th to 25th, with the REMIR Camera (field of view of 10'x10' and a pixel size of 1.22") mounted on REM, a 60-cm robotic telescope located at the La Silla Observatory (Chile).
We detect only one source in a 4" error circle around the Swift XRT position (Campana et al., ATEL #688), coincident with a 2MASS catalogued source, having the following magnitudes:
J = 13.47 +/- 0.03 H = 12.95 +/- 0.05 K = 12.59 +/- 0.07
The source magnitudes calibrated on the 2MASS itself are fully consistent with the 2MASS values, all the measurements giving differences below 0.1 mag, well within 1-sigma uncertainties. The differences between our measurements and the 2MASS magnitudes for the nights of January 20, 21 and 22 are reported in http://www.sron.nl/~nanda/swift1626.html . Our 3-sigma detection upper limits are J < 16.66, H < 15.75 and K < 15.29 .
Although this is the only infrared source in the X-ray error circle we cannot unambiguously identify it as the infrared counterpart of SWIFT J1626.6-5156, because no significant infrared variability was detected which might have followed the X-ray outburst, and the XRT error circle is not small enough to statistically claim it as the right counterpart.
In any case, we can reliably say that the infrared magnitudes are too faint for the star being a Supergiant or a Be type star. Furthermore, after de-reddening (using the Nh~0.9x10^21 measured by the XRT and Predehl & Schmitt 1995) the infrared and optical magnitudes (optical magnitudes derived from the DENIS database, I=14.58, R=15.9 and B=17.7), the source colours appear extremely red and highly inconsistent with an O or B type star (Cox 2002). On the other hand, with an Nh~0.9x10^21 cm^-2, any other star of these spectral types, even if at the edge of the Galaxy, should have been detected in the infrared band within our upper limits. This reliably rules out the possibility of SWIFT J1626.6-5156 being a canonical high mass X-ray binary pulsar. This makes this object a probable low mass X-ray binary hosting a slowly rotating pulsar.
A more accurate determination of the SWIFT J1626.6-5156 position is needed in order to continue the investigation in the infrared and optical bands with bigger telescopes. | 2006-01-27 18:56:00 | infra-red,optical,x-ray,binary,pulsar,star,transient,request for observations | 2006-01-27 | 18:56:00 | 2,698 | [
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] | 712 |
714 | Bright New Black Hole Transient XTE J1817-330 | R. Remillard, A. M. Levine, E. H. Morgan (MIT), C. B. Markwardt (U. Maryland & NASA/GSFC), & J. H. Swank (NASA/GSFC) | We report a new source discovered by the RXTE ASM and follow-up observations with the RXTE PCA.
Observations with the RXTE All-Sky Monitor on 2006 Jan. 26 suggested the sudden appearance of a very bright X-ray source near ra=274.56, dec=-32.92 (degrees, J2000). The angular proximity to the sun limited the number of dwells and the position accuracy. The (2-12 keV) flux was 0.93 (0.03) Crab, compared to an upper limit (3 sigma) of 0.05 mCrab on Jan. 25. The spectrum appeared very soft, as frequently exhibited by black hole candidates.
The RXTE PCA pointed at the ASM position Jan 27 at 21 UT and confirmed the presence of a bright soft source. On Jan 28 at 14 UT the PCA scanned over the position and determined a position of ra=274.425, dec=-33.018, for which the systematic errors should be less than 30" (Jahoda et al. 2006). The spectrum exhibits little absorption (< 10^ 21 cm^-2). For both observations it can be described by black body contributions at about 0.8 and 0.4 keV and a powerlaw with photon index of 2-3. The fluxes were 1.2 and 1.35 Crab(2-10 keV), respectively, and 15 and 22 mCrab (10-30 keV). Source rms variability was only 1.3% during 900 seconds of observation. | 2006-01-29 05:32:00 | x-ray,black hole,the sun,transient | 2006-01-29 | 05:32:00 | 1,192 | [
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] | 713 |
715 | The symbiotic star CD-57 3057 is the likely counterpart of IGR J10109-5746 | N. Masetti, L. Bassani (IASF/INAF, Bologna), A. J. Dean (Univ. Southampton), P. Ubertini (IASF/INAF, Rome) and R. Walter (ISDC, Versoix) | We report that, further to the discovery of the new INTEGRAL source IGR J10109-5746 belonging to the Crux Galactic arm survey (Revnivtsev et al. 2005, astro-ph/0508155) and of its likely soft X-ray counterpart SWIFT J1010.1-5747 (Tueller et al., ATel #669), a SIMBAD catalog search showed that the precise Swift/XRT source position is consistent with the emission-line late-type star CD-57 3057.
Inspection of the published optical spectrum of this star (Pereira et al., 2003, A&A, 397, 927) suggests strong similarities with that of RT Cru, the optical counterpart of IGR J12349-6434 (see ATels #519, #528, #591).
Therefore, given the positional coincidence of the INTEGRAL, Swift and optical sources described above, we conclude that CD-57 3057 is the likely optical counterpart of IGR J10109-5746, and that it is a symbiotic system similar to IGR J12349-6434/RT Cru.
This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France. | 2006-01-31 01:26:00 | optical,x-ray,binary,cataclysmic variable,star,variables,a comment | 2006-01-31 | 01:26:00 | 960 | [
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] | 714 |
716 | Multiple Photometric Periods in SXP1323 (RX J0103.6-7201) | Paul C. Schmidtke and Anne P. Cowley (Arizona State University) | RX J0103.6-7201 (SXP1323) is a Be/neutron-star binary in the Small Magellanic Cloud with the longest known X-ray pulsation period (1323 s; Haberl & Pietsch 2005, A&A, 438, 211). The optical counterpart is #1393 from the emission-line catalogue of Meyssonnier & Azzopardi (1993, A&AS, 102, 451). Periodogram analysis of OGLE-II photometric data for this 14th magnitude star reveals three strong periodicities at 26.16 d, 0.88 d, and 0.41 d. All show approximately sinusoidal light curves with full amplitudes of 0.045, 0.035, and 0.03 mag, respectively. The analysis is complicated since all of these periods, as well as their aliases, are present simultaneously. We have divided the data into four seasons to search for changes in the periods or amplitudes, but they appear to be stable. The two shorter periods are most likely due to non-radial pulsations of the Be star, of the type seen in several other Be/neutron-star X-ray sources. The 26-d period is difficult to understand, since it is shorter than would be expected from the pulsation/orbital period relation for Be/X-ray binaries (e.g. Corbet 1984, A&A, 141, 91). Furthermore, the sinusoidal shape of the light curve argues against it being an orbital period, since generally such light curves show brief optical (and/or X-ray) outbursts as the neutron star passes periastron, rather than a smooth sinusoidal variation. An alternate interpretation is that the strong 26-day period is the alias of a shorter non-radial pulsation period at either 0.96 or 1.04 days, but the power is weaker at these periods. Further data are needed to resolve this ambiguity. | 2006-01-31 02:49:00 | optical,x-ray,binary,neutron star,pulsar,star,variables | 2006-01-31 | 02:49:00 | 1,616 | [
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] | 715 |
717 | Possible Radio Counterpart to XTE J1817-330 | M. P. Rupen V. Dhawan, A. J. Mioduszewski (NRAO) | Very Large Array (VLA) observations of the black hole candidate binary XTE J1817-330 (ATel #714) on 31 January 2006 show one radio source within the 30-arcsec RXTE PCA error box, at a J2000 position of: 18h 17m 43.537s -33d 01' 07.8" As these data were taken shortly after an array reconfiguration, the astrometric uncertainty is dominated by the poorly-known positions of the newly-moved antennas, giving a current uncertainty of a few tenths of an arcsecond. This can be improved once the antenna positions are measured more accurately. The 4.86 and 8.46 GHz data are consistent with an unresolved source, the beam sizes being 1.1 x 0.4 arcsec and 0.6 x 0.2 arcsec respectively (both oriented about 5 degrees west of north).
The flux densities were 2.1 +/- 0.3 mJy at 1.40 GHz; 0.83 +/- 0.12 mJy at 4.86 GHz; and 0.58 +/- 0.11 mJy at 8.46 GHz. The radio spectrum thus goes as frequency to the power -0.73+/-0.13. There is no source in the 1.4 GHz NRAO VLA Sky Survey (NVSS; Condon et al. 1998, AJ 115, 1693): the nominal flux density at the position of the source is 0.7 +/- 0.5 mJy/beam.
Given the rarity of unresolved sources at these frequencies, it seems likely that this is the radio counterpart to XTE J1817-330. However, the evidence for variability so far is marginal (2.4 sigma). If this is indeed the radio counterpart, the steep spectrum suggests we are seeing the decaying tail of an outburst. Further VLA observations are planned.
The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. | 2006-02-01 13:54:00 | radio,binary,black hole,transient | 2006-02-01 | 13:54:00 | 1,608 | [
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718 | TT Ari: Recent Negative Superhumps and QPO's | J. N. Yoon (CBNU, Korea), I. L. Andronov (ONU, Ukraine), S. M.Cha (CBNU, Korea), | TT Ari has been recently discovered to be at a relatively unstable phase by Andronov, Gazeas & Niarchos (2005, VSNET-Campaign 1630). Its prolonged "positive superhump" state from 1997 to 2004 has changed. In October-November, 2005, the star was fainter, and the superhumps are not pronounced. The dominating type of variability was quasi-periodic oscillations (QPO) with a time-scale of 10-35 minutes and amplitude 0.07 mag (B). This state is distincly different from both the bright "negative superhump" state and the "positive superhump" state (Andronov et al. IBVS, 2005, N 5664). Further monitoring had been carried out at the 40-cm telescope of the University Observatory, Chungbuk National University, Cheongju, Korea. From October 25, 2005 to January 24, 2005, alltogether 11245 data points have been obtained during 37 nights using the R filter with a time resolution 34-70 sec. Yoon, Andronov, Cha & Kim (2005, VSNET-Campaign 1636, ATel 698) reported on the "outburst-like" event with an amplitude of 0.9m (R) and characteristic timescales dt/dm=15.87(11)days/mag (rise at JD 2453704-715) and dt/dm=4.95(7)days/mag (fall at HJD 2453721-724). Then there was a standstill with minor fluctuations of the mean brightness. Yoon, Andronov, Cha, Chinarova & Kim (2005, VSNET-Campaign 1637 reported on a standstil with a mean level =10.732 and a scatter of 0.107 mag, which is much larger than an error estimate 0.020 mag. The "Lambda-scalegram" analysis (Andronov 2003, ASP CS 292,391) shows a most prominent peak corresponding to the QPO with an effective period of 0.01439d=20.7min and semi-amplitude of 0.061mag. The superhump variability is less prominent (semi-amplitude 0.033mag and period 0.128d). This is typical for the "negative superhump" state observed before 1997 (Tremko et al. 1996, AA 312, 121; Andronov et al. 1999, AJ 117, 574). Similar periods (0.01486d, 0.1166d) are present at the sine-based periodogram ( Andronov 1994, OAP 7, 49), but the corresponding peaks are low enough arguing for a quasi-periodic character of variations, rather than truly periodic. The long-term light curve and nightly mean are presented. The character of variability seems to be changed again. A recent light curve started at JD 2453742.8 shows both negative superhumps and QPOs. The periodogram shows the higher semi-amplitude of superhumps (77+-5mmag) then that of the QPOs (50+-4mmag). The ephemeris for this night is Max.HJD=2453743.00362(21)+0.015098(44)*E corresponding to unexpectedly high coherence of these 20-min pulses during this night. From 16 individual timings of maxima, we determined a consistent value 0.0158d. One should note the presence of other maxima, which are often more thin and occur at different phases of the QPO period, sometimes splitting the maxima. For the 3-hour variability, we have determined 12 minima timings, which have been analyzed using the PERMIN algorithm (Andronov 1991, KFNT 7, 2, 78). The corresponding periodogram has a minimal phase scatter for the elements Min.HJD=2453747.0700(47)+0.132322(53)*E. This is slightly different (by 4.5 sigma) from the period obtained from the sine fit P=0.1217(22)d, but the light curve definitely shows cycle-to-cycle changes, so this difference seems not to be statistically significant. Spectral and multi-color photometric observations of TT Ari at this state of multi-component variability are requested. | 2006-02-02 06:11:00 | optical,cataclysmic variable,star,variables,request for observations | 2006-02-02 | 06:11:00 | 3,391 | [
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] | 717 |
719 | Optical identification of IGR J13091+1137 as a heavily obscured AGN | N. Masetti, E. Palazzi, A. Malizia (INAF-IASF, Bologna), A. J. Bird (Univ. Southampton), L. Norci (Dunsink Obs.), I. Bruni (INAF-Oss. Astron. Bologna), A. Bazzano and A. De Rosa (INAF/IASF, Rome) | In order to identify the nature of the active nucleus of spiral galaxy NGC 4992, associated with the Chandra and INTEGRAL high-energy sources CXOU J130905.6+113803 and IGR J13091+1137 (see Halpern, Atel #572 and Sazonov et al., 2005, A&A, 444, L37), we acquired a 15-minute optical spectrum on February 1, 2006 with the instrument BFOSC mounted on the `G.D. Cassini' 1.5m telescope of the Astronomical Observatory of Bologna located in Loiano (Italy).
The spectral continuum in the range 4000-8000 Angstroms is typical of a normal spiral galaxy, with CaII H+K doublet, G-band at 4304A, Hbeta, Mg b band at 5175A, FeI at 5270A and NaI doublet at 5890A absorptions, and a weak [NII] 6583A emission. All of these features are at a redshift z = 0.025 (consistent with that reported on the Hyperleda catalogue).
The X-ray (0.5-8 keV) luminosity (1.2*10^42 erg cm-2 s-1; Sazonov et al. 2005) combined with the optical spectrum properties suggests that NGC 4992 belongs to the class of X-ray Bright, Optically Normal Galaxies (XBONGs; e.g., Comastri et al. 2002, astro-ph/0203019; see also Severgnini et al. 2003, A&A, 406, 483). The intrinsic absorption measured by Chandra and the INTEGRAL detection further indicate that in this case the best explanation for the nature of this source is a heavily absorbed AGN. To the best of our knowledge, this is the first XBONG detected at energies above 20 keV, and its closeness to Earth makes NGC 4992 an ideal laboratory for the study of this enigmatic class of galaxies.
We acknowledge the Astronomical Observatory of Bologna for the Service Programme in Loiano. | 2006-02-03 22:42:00 | optical,x-ray,agn | 2006-02-03 | 22:42:00 | 1,604 | [
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] | 718 |
720 | Swift observations of Swift J0911.2+4533 | D. Grupe (PSU), J. Tueller (NASA/GSFC), C. Markwardt (U Md, NASA/GSFC), J. A. Kennea (PSU), A. Falcone (PSU), R. Mushotzky (NASA/GSFC), S. Barthelmy (NASA/GSFC), H. Krimm (NASA/GSFC), S. Campana (OAB), O. Godet (U Leicester), G. K. Skinner (CERS), K. Mukai (NASA/GSFC), S. T. Holland (NASA/GSFC), M. Ajello (MPE), J. Greiner (MPE), and T. Belloni (INAF) | We report on the X-ray detection in the 0.3-10 keV band of Swift J0911.2+4533. The source was detected in our ongoing Swift Burst Alert Telescope (BAT) hard X-ray survey (Tueller et al. ATEL #668 and #669, Kennea et al. ATEL #677, Ajello et al. ATEL #697). Swift J0911.2+4533 was observed on 2006-01-04 01:16 (UT start time) for a total of 5.5 ks and on 2005-01-07 17:36 (UT start time) for 8.9 ks with the X-ray Telescope (XRT) and UV/Optical Telescope (UVOT) on board Swift. We found a faint X-ray source at RA (2000) = 09 11 29.91 Dec (2000) = +45 28 02.1 with a position error of 4.0".
The position of this source coincides with 2MASX J091129.9+452806. Optical spectroscopy from the SDSS displays very strong [OIII] and [NII] emission lines which classify this source as a Seyfert 2 galaxy with a redshift z=0.0268. A combined power law fit to the BAT and XRT data shows that the X-ray spectrum of this AGN is highly absorbed with a column density of 3.7+1.8/-1.3 e23 cm-2 and a Photon index Gamma = 3.0+1.2/-0.8. The absorbed 0.2-10.0 keV flux is 1.7e-12 ergs/s/cm2, and corrected for absorption 1.5e-10 ergs/s/cm2. The intrinsic 0.2-10 keV luminosity is 3e44 ergs/s. The flux in the 15-150 keV band is 1.8e-11 ergs/s/cm2.
Swift J0911+4533 was not detected in the ROSAT All-Sky Survey in the 0.1-2.0 keV band, suggesting that it was also absorbed at the time of the RASS coverage in October 1990. This region was not observed by any other X-ray mission, either.
The UVOT analysis confirmed the strong reddening of this Seyfert 2 galaxy. We found the following magnitudes in the 6 UVOT filters:
V: 15.83+/-003
B: 16.89+/-0.06
U: 17.10+/-0.06
UVW1: 18.27+/-0.08
UVM2: 19.18+/-0.11
UVW2: 19.17+/-0.07
The UVOT image and the SDSS images suggest that the galaxy is viewed edge-on. | 2006-02-04 00:02:00 | optical,ultra-violet,x-ray,agn | 2006-02-04 | 00:02:00 | 1,790 | [
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] | 719 |
721 | Confirmation of Radio Counterpart to XTE J1817-330 | M. P. Rupen V. Dhawan, A. J. Mioduszewski (NRAO) | Very Large Array (VLA) observations of the black hole candidate binary XTE J1817-330 (ATel #714) show that the suggested radio counterpart (ATel #717) has faded significantly (3.9sigma) at 4.86 GHz, from 0.83 +/- 0.12 mJy on Jan. 31 to 0.32 +/- 0.06 mJy on Feb. 2, and 0.35 +/- 0.05 mJy on Feb. 3. This variability strongly suggests that this is indeed the counterpart to the X-ray transient.
The Feb. 3 observations, using newly-determined antenna positions, also yield an improved (J2000) position for the source: 18h 17m 43.526s -33d 01' 07.47" with a likely accuracy of +/- 0.2 arcseconds.
The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. | 2006-02-04 05:21:00 | radio,x-ray,binary,black hole,transient | 2006-02-04 | 05:21:00 | 755 | [
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] | 720 |
722 | Radio Observations of SN 2005ke | Alicia Soderberg (Caltech) | I observed the peculiar SN 2005ke in NGC 1371 (IAUC 8630 , CBETs 291,387) with the Very Large Array on 2005 November 18.2 and 2006 January 27.1 UT. No radio emission is detected at the optical position at in either epoch at an observing frequency of 8.46 GHz. Further observations are planned. | 2006-02-06 02:01:00 | radio,optical,supernovae | 2006-02-06 | 02:01:00 | 293 | [
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] | 721 |
723 | Discovery of four SN candidates as a part of A Survey for Supernovae in Massive High-Redshift Clusters | K. Sharon (Tel Aviv University), Avishay Gal-Yam (Caltech) and D. Maoz (Tel Aviv University) | K. Sharon (Tel Aviv U.), A. Gal-Yam (Caltech), and D. Maoz (Tel Aviv U.) report for a larger collaboration, including M. Donahue (MSU), H. Ebeling (IfA), R. Ellis (Caltech), A. Filippenko (UCB), R. Foley (UCB), W. Freedman (OCIW), J.-P. Kneib (Marseille), R. Kirshner (CfA), T. Matheson (NOAO), J. Mulchaey (OCIW), M. Phillips (OCIW), V. Sarajedini (UF) and M. Voit (MSU) (http://www.astro.caltech.edu/~avishay/hst.html): We have used the Advanced Camera for Surveys (ACS) on board the Hubble Space Telescope (HST), to image the galaxy clusters CL1226+3332 (z=0.888) and MACS 0647+7015 (z=0.584) for one orbit each (2209s and 2584s respectively) with the F814W filter, as part of our cycle 14 survey for SNe in galaxy clusters (GO 10493, PI Gal-Yam). Comparing our new data for CL1226+3332 (2006 Jan 29.5 UT) with previous archival observations (2003 Apr 13.5 UT, GO 9033, PI Ebeling), and our new data for MACS 0647+7015 (2006 Feb 1.0 UT) with previous archival observations (2004 Dec 5.0 UT, GO 9722, PI Ebeling), we detect 4 transient point sources (two in each cluster). The discovery dates, coordinates and magnitudes are listed in the table below. Name Coordinates (RA, Dec; J2000.0) Discovery (Date, Mag) Host (RA, Dec, Offset, Mag) CL1226_1 12:26:54.507 +33:33:58.28 Jan06 25.75 12:26:54.473 +33:33:58.14 0.55''E 0.16''N 20.53 CL1226_2 12:26:55.460 +33:32:14.31 Apr03 24.01 12:26:55.545 +33:32:14.66 1.05''E 0.35''N 20.16 MACS0647_1 06:47:30.025 +70:14:54.71 Feb06 25.84 06:47:29.863 +70:14:54.39 0.82''E 0.32''N 22.54 MACS0647_2 06:47:38.030 +70:16:16.72 Dec04 26.78 06:47:38.041 +70:16:16.10 0.05''E 0.62''N 22.20 We note that the coordinates we cite are based on the HST WCS information and should be regarded as preliminary. The lack of detectable proper motion over the span of the observations argues against a solar-system origin, and the offsets from galaxy cores clearly rule out AGN. We therefore conclude that these new sources are most likely SNe. | 2006-02-07 02:17:00 | optical,agn,supernovae,transient | 2006-02-07 | 02:17:00 | 1,967 | [
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] | 722 |
724 | Discovery of the NIR counterpart of XTE J1817-330 | P. D'Avanzo (INAF-OAB), P. Goldoni (CEA, Saclay), S. Covino (INAF-OAB), S. Campana (INAF-OAB), E. Molinari(INAF-OAB), G. Chincarini (Uni. Bicocca), F. M. Zerbi (INAF-OAB), V. Testa (INAF-OAR), G. Tosti (Uni. Perugia), F. Vitali (INAF-OAR), L. A. Antonelli (INAF-OAR), P. Conconi (INAF-OAB), G. Malaspina (INAF-OAB), L. Nicastro (INAF-IASF-Pa), E. Palazzi (INAF-IASF-Bo), on behalf of the REM/ROSS Team | We report on optical and infrared observations of the black hole candidate XTE J1817-330 (ATel #714). The observations were performed in the K band with the REMIR Camera (field of view of 10'x10' and a pixel size of 1.22") and in the R band with the ROSS Camera (field of view of 10'x10' and a pixel size of 1.22"). Both instruments are mounted on REM, a 60-cm robotic telescope located at the La Silla Observatory (Chile). NIR observations started on Feb 7.378 (UT), for a total of 10 minutes of exposure. We find a source at the position: R.A.(2000) = 18:17:43.54 Dec.(2000) = -33:01:06.7 with an accuracy of +/- 0.5 arcseconds. This position is consistent with the position of the radio counterpart (ATel #721). The magnitude of the object is K = 15.0 +/- 0.4, calibrated with respect to the 2MASS catalogue. Further analysis is in progress. We propose this source as the NIR counterpart of XTE J1817-330. A finding chart can be found at the following URL: www.merate.mi.astro.it/~davanzo/REM/XTE_J1817/XTE_REMIR_2MASS_K_3.jpg | 2006-02-07 22:29:00 | radio,infra-red,optical,binary,black hole,transient | 2006-02-07 | 22:29:00 | 1,029 | [
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] | 723 |
725 | Continuing RXTE observations of XTE J1701-462: a new "Z" in town? | Jeroen Homan (MIT), Tomaso Belloni (INAF/OAB), Michiel van der Klis, Piergiorgio Casella (U. Amsterdam), Mariano Mendez (SRON), Walter Lewin (MIT), Rob Fender (U. Southampton), Elena Gallo (UCSB), and Neil Gehrels (NASA/GSFC) | Since January 19 the new X-ray transient XTE J1701-462 (ATels #696, #703, #708, #710) has been observed more than 45 times with the Rossi X-ray Timing Explorer (RXTE). Preliminary analysis of the RXTE data suggest the source is a neutron star LMXB and is currently showing behavior typical of the so-called "Z sources" (i.e. the brightest, persistent neutron star LMXBs). This would make XTE J1701-462 the first new Z source in nearly 35 years.
The prospect of XTE J1701-462 of being a transient Z source opens up interesting possibilities if the source eventually fades away. A major question that can be addressed is whether at lower mass accretion rates Z sources start to behave like atoll sources. Regardless of these future opportunities, XTE J1701-462 already is a unique and interesting source and we strongly urge observers to continue or start monitoring the source at all wavelengths. For those who are interested a detailed description of the RXTE observations is given below.
For figures, visit: http://tahti.mit.edu/Z
RXTE/PCA light curves reveal that the source continues to exhibit large count rate changes (by factors of more than two on a time scale of hours). However, occasionally the count rate can be relatively stable for periods of ~1 day. The count rate changes are often accompanied by large changes in the X-ray colors, especially above 8 keV.
In a color-color diagram (CCD) these spectral changes result in a multi-branched track that resembles those of some of the neutron star Z sources, in particular that of GX 5-1 (see figure 13 in Jonker et al. 2002, MNRAS, 333, 665). In the plot of our CCD we tentatively identify some of the branches as the horizontal branch (with strong upturn), the normal branch, and the flaring branch (with a dipping branch, as also seen in GX 5-1). Over the course of our observing campaign the overall position of the track has shifted to slightly softer colors. Such shifts are not uncommon in Z sources. These shift are even more apparent in color-intensity diagrams (CIDs). The sharp turn that we identify as the horizontal/normal branch vertex has slowly increased in count rate during the past two and a half weeks, suggesting that the source has increased in brightness by more than 20%. We also note that the flaring branch is inverted - this is particularly clear when plotting count rate vs. soft X-ray color. Such behavior has previously been seen before in the Z source Cygnus X-2.
The rapid X-ray variability properties of the source evolve smoothly along the track in the CCD/CID (see link above for example power spectra). At the start of the horizontal branch (upturn) we detect a ~10 Hz QPO that smoothly increases in frequency along the horizontal branch onto the top normal branch where it reaches a maximum of ~55 Hz (see also ATel #703). This QPO is accompanied by band limited noise that also increases in frequency. Both QPO and noise decrease in strength as their frequencies increase. Around the middle of the normal branch we detect a broad feature near 5-6 Hz (see also ATel #703), which is particularly clear in power spectra above 8 keV. The feature disappears near the bottom of the normal branch. On the flaring branch the power spectrum only shows weak red noise (rms variability [0.1-100 Hz] is ~2.5%, compared to 16% on the top of the horizontal branch).
The evolution of the timing features along the tracks in the CCD/CID as well as their typical strength and frequency are very similar to those seen in the Z sources. The relatively weak power-law component in the energy spectra further supports the link with the Z sources. Other neutron star signatures, like X-ray bursts, pulsations, or kHz QPOs have not been detected so far. | 2006-02-08 20:50:00 | x-ray,binary,neutron star,star,transient | 2006-02-08 | 20:50:00 | 3,733 | [
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] | 724 |
726 | Swift Observations of Supernova 2006X in M100 | Stefan Immler (NASA/USRA/GSFC) | S. Immler, Goddard Space Flight Center, NASA and Universities Space Research Association, P. Brown, Pennsylvania State University, and Peter Milne, U. of Arizona, on behalf of the Swift-satellite team, report on Swift Ultraviolet/Optical Telescope (UVOT; wavelength range 170-650 nm) and X-Ray Telescope (XRT; 0.2-10 keV) observations of the Type Ia SN 2006X (CBET #393) obtained on Feb 8.33 UT.
A new optical/UV source is detected at R.A. = 12h22m53s.92, Decl. = +15o48'31".2 (equinox 2000.0), when compared to Swift UVOT observations obtained on Nov 13, 2005, consistent with the Lick Observatory position reported in IAUC # 8667 . UVOT magnitudes are V = 15.7 mag (165 s exposure), B = 17.2 mag (103 s), U = 18.0 mag (165 s), UVW1 [181-321 nm] = 18.2 mag (332 s), UVM2 [166-268 nm] = 19.2 mag (506 s), and UVW2 [112-264 nm] > 20.4 mag (3-sigma upper limit; 674 s). Statistical and systematic errors are 0.1 mag each.
No X-ray source is detected at the position of SN 2006X in a simultaneous 2,124 s XRT X-ray observation. The 3-sigma upper limit to the (0.2-10 keV band) count rate is 4.9E-03 cts/s, corresponding to an X-ray flux and luminosity of <2.7E-13 ergs/cm/cm/s and <9.3E39 ergs/s, respectively, for an assumed thermal plasma spectrum with a temperature of 10 keV and an absorbing foreground column density of 2.39E+20 cm**-2 (Dickey & Lockman 1990, ARAA 28, 215). Further Swift observations are scheduled. | 2006-02-09 15:30:00 | optical,ultra-violet,x-ray,supernovae | 2006-02-09 | 15:30:00 | 1,420 | [
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] | 725 |
727 | A radio flare from Cyg X-3 | Tsuboi (NRO NAOJ), N. Kuno (NRO NAOJ), T. Umemoto (NRO NAOJ), T. Sawada (NRO NAOJ), K. Nakanishi (NRO NAOJ), T. Tosaki (NRO NAOJ), Y. Kurono (NRO NAOJ), K. Fujisawa (Yamaguchi-U), Japanese VLBI Network Team, S. Trushkin (SAO RAS), T. Kotani (Tokyo Tech), N. Kawai (Tokyo Tech) | We report that the microquasar Cyg X-3 is undergoing a significant radio flare and would request for followup observations at all frequencies. In the current multi-frequency monitoring observations with RATAN-600 radio telescope, the flux density at 4.8 GHz of the source was found to drop from 103 mJy on Jan 14.4 (UT) to 43 mJy on Jan 15.4 (UT), and to 22 mJy on Jan 17.4 (UT). The source is known to exhibit the radio flares typically with a few peaks exceeding 5 Jy following such quenched state (Waltman et al., 1994, AJ, 108, 179). The source has been monitored from Jan 25 (UT) with the Nobeyama Radio Observatory 45m Telescope (NRO45m Telescope), the Nobeyama Millimeter Array (NMA), Yamaguchi-University 32-m Radio Telescope (YRT32m), and Japanese VLBI Network telescopes. On Feb 2.2 (UT), about 18 days after it entered the quenched state, the rise of a first peak is detected with the NRO45m Telescope and YRT32m. On Feb 3.2 (UT), the flux densities reached to the first peak at all the sampling frequencies from 2.25 GHz to 110.10 GHz. The typical flux is 1 - 1.2 Jy and the peak spectrum is flat over the observation band, suggesting an optically thick radio source. The peak spectrum and light curves are plotted respectively here: http://www.hp.phys.titech.ac.jp/kotani/cygx3/11.html and http://www.hp.phys.titech.ac.jp/kotani/cygx3/7.html The current RATAN-600 simultaneous spectra (1-30 GHz) are plotted at: http://cats.sao.ru/~satr/XB/CygX-3/CygX-3_Feb2006sp.gif
After the peak, the flux densities decayed exponentially (or power-law) with a time scale of 4-8 days, except for rapid variation of more than 100 mJy in 30 min. On Feb 8.90 (UT), the rise of a second peak was detected with the NRO45m Telescope. During 1 hour the flux density increased from 900 mJy to 1340 mJy at 23 GHz. On Feb 9.5 (UT) the RATAN-600 indicated from 400 mJy at 2.3 GHz to 545 mJy at 30 GHz.
Further observations are in progress. | 2006-02-09 18:40:00 | radio,millimeter,binary,black hole,request for observations | 2006-02-09 | 18:40:00 | 1,929 | [
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728 | Radio Observations of Type Ia SN2006X | Alicia Soderberg (Caltech) | Alicia Soderberg (Caltech) reports: I observed the Type Ia supernova 2006X in NGC 4321 (IAUC 8667 , CBET 393) with the Very Large Array on 2006 February 9.34 UT (approximately 2 days after optical discovery). The 2.5 hour observation at 8.46 GHz reveals no radio source coincident with the optical SN position. I place a limit on the radio flux density of 45 microJy (3 sigma). At a distance of 16 Mpc this limit corresponds to a luminosity of 1.4 x 10^25 erg/s/Hz. I am grateful to the VLA scheduling officers and operators for making this target of opportunity observation possible. | 2006-02-09 23:53:00 | radio,optical,supernovae | 2006-02-09 | 23:53:00 | 584 | [
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] | 727 |
729 | SUPERNOVA 2006X IN NGC 4321 (M100) | C. J. Stockdale and M. Kelley, Marquette University; R. A. Sramek, National Radio Astronomy Observatory; S. D. Van Dyk, Spitzer Science Center, California Institute of Technology; S. Immler, Goddard Space Flight Center and Universities Space Research Association; K. W. Weiler and C. L. M. Williams, Naval Research Laboratory; and N. Panagia, Space Telescope Science Institute | We report the lack of detection of radio emission near the position of the type-Ia supernova 2006X (IAUC 8667 , CBET 393) with the Very Large Array: âUpper limits (3 sigma) to any radio flux density were established on 2006 Feb. 09.37 UT of <0.162 mJy (Spectral Luminosity < 5.6 x 10^25 erg/s/Hz) at 22.460 GHz (wavelength 1.3 cm) and <0.047 mJy (Spectral Luminosity < 1.5 x 10^25 erg/s/Hz) at 8.460 GHz (wavelength 3.5 cm), among the deepest and earliest limits yet obtained for radio emission from a type Ia supernova. Under standard assumptions, this implies a mass loss rate from the presupernova system of < few x 10^-8 Msun/yr. The search for radio emission was conducted within ~10â of the published optical position of SN 2006X (R.A. = 12h22m53.s99, Decl. = +15o48â33â.1, equinox 2000.0; IAUC 8667 ) and no radio emission was detected near the supernova position exceeding three times the map rms at any of the times or in any of the frequency bands listed.â | 2006-02-10 00:26:00 | radio,optical,supernovae | 2006-02-10 | 00:26:00 | 976 | [
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730 | SN 2006U is an AGN | The Nearby Supernova Factory: N. Blanc, Y. Copin, E. Gangler, G. Smadja (Institut de Physique Nucleaire de Lyon), P. Antilogus, S. Gilles, R. Pain, R. Pereira (Laboratoire de Physique Nucleaire et de Haute Energies de Paris), G. Aldering, S. Bailey, S. Bongard, D. Kocevski, B. C. Lee, S. Loken, P. Nugent, S. Perlmutter, R. Scalzo, R. C. Thomas, L. Wang, B. A. Weaver (Lawrence Berkeley National Laboratory, Berkeley, CA), E. Pecontal, G. Rigaudier (Centre de Recherche Astronomique de Lyon), R. Kessler (Kavli Institute for Cosmological Physics, Chicago, IL), C. Baltay, D. Rabinowitz, A. Bauer (Yale) | The Nearby Supernova Factory reports that a spectrum (range 320-1000 nm) of SN2006U (IAUC # 8667 ), obtained 2006 February 8.4 UT with the Supernova Integral Field Spectrograph on the University of Hawaii 2.2-meter telescope, shows it to be an AGN at redshift 0.25. The redshift was determined by matching H-alpha and H-beta to the SDSS composite AGN template (Vanden Berk et al., 2001, AJ, 122, 549). | 2006-02-10 08:57:00 | infra-red,optical,ultra-violet,agn,supernovae | 2006-02-10 | 08:57:00 | 401 | [
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] | 729 |
731 | INTEGRAL detects hard X-ray emission from XTE J1817-330 | S. E. Shaw (Southampton, UK/ ISDC, Geneva); J. Zurita (ISDC, Geneva); E. Kuulkers (ESA/ESAC, Spain); S. Brandt, J. Chenevez (DNSC, Denmark); T. J.-L. Courvoisier (ISDC, Geneva); K. Ebisawa (NASA/GSFC, USA); P. Kretschmar (ESA/ESAC, Spain); C. Markwardt (NASA/GSFC, USA); N. Mowlavi (ISDC, Geneva); T. Oosterbroek (ESA/ESTEC, Netherlands); A. Orr (ESA/ESTEC, Netherlands); A. Paizis (IASF, Milano); C. Sanchez-Fernandez (ESA/ESAC, Spain); R. Wijnands (UvA, Netherlands) | During the start of the third period of the INTEGRAL Galactic Bulge monitoring observations (Kuulkers et al 2005, ATel #438), the X-ray transient and black-hole candidate XTE J1817-330 (ATel #714) has been detected in the 20 - 150 keV range. The observations comprised ~7 ksec taken on 9 Feb 2006 between 09:02 and 11:43 UTC.
The estimated flux seen by ISGRI in the 20-60 keV range was ~33 mCrab, which compares with an earlier measurement, on 27 Jan 2006, of 22 mCrab in the 10-30 keV band (ATel #714). There is also evidence of emission at higher energies, with an average flux in the 60-150 keV band of 1.9 ± 0.4 cps (~ 44 mCrab). Spectral analysis indicates a hard spectrum with a power-law photon index of 1.6 +/- 0.3.
Unfortunately, the source was outside of the field of view of the JEM-X instrument and so no comment can be made on the sources's behaviour below 15 keV.
Images and light curves from the observations are available at
http://isdc.unige.ch/Science/BULGE
The source will again be observed by INTEGRAL in the next Galactic Bulge pointing on 11-12 Feb 2006. A longer (195 ksec) INTEGRAL TOO observation is foreseen on 15-18 Feb, 2006.
Simultaneous observations are encouraged. | 2006-02-10 18:38:00 | x-ray,gamma ray,black hole,transient,a comment | 2006-02-10 | 18:38:00 | 1,202 | [
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] | 730 |
732 | Discovery of SNF20060208-004 (Type II), Classification of SN 2006aa (Type IIn) and SN 2006ac (Premaximum Type Ia) | The Nearby Supernova Factory: N. Blanc, Y. Copin, E. Gangler, G. Smadja (Institut de Physique Nucleaire de Lyon), P. Antilogus, S. Gilles, R. Pain, R. Pereira (Laboratoire de Physique Nucleaire et de Haute Energies de Paris), G. Aldering, S. Bailey, S. Bongard, D. Kocevski, B. C. Lee, S. Loken, P. Nugent, S. Perlmutter, R. Scalzo, R. C. Thomas, L. Wang, B. A. Weaver (Lawrence Berkeley National Laboratory, Berkeley, CA), E. Pecontal, G. Rigaudier (Centre de Recherche Astronomique de Lyon), R. Kessler (Kavli Institute for Cosmological Physics, Chicago, IL), C. Baltay, D. Rabinowitz, A. Bauer (Yale) | The Nearby Supernova Factory reports the discovery of SNF20060208-004 (RA 09:07:43.11 Dec. +12:03:06.5 J2000.0) in images obtained February 8.3 UT with an approximate magnitude of 18.9 (calibrated to R) using the QUEST II camera on the Palomar Oschin 48-inch telescope as a part of the JPL Near-Earth Asteroid Tracking component of the Palomar Consortium. A spectrum (range 320-1000 nm) of this object obtained February 10.5 UT with the Supernova Integral Field Spectrograph on the University of Hawaii 2.2-meter telescope, shows it to be a Type II supernova at an approximate redshift of z = 0.03, as measured from the peak of its H-alpha emission.
The Nearby Supernova Factory also reports classifications for supernovae 2006aa and 2006ac (both IAUC # 8669 ) using SNIFS spectra taken February 10.5 and 10.6 UT respectively. SN 2006aa is a Type IIn supernova at an approximate redshift measured from its H-alpha emission peak of z = 0.02, consistent with that of its host (NGC 3947 at z = 0.020671, de Vaucouleurs et al. 1991, RC3.9 via NED). SN 2006ac is a young Type Ia supernova, similar to SN 1994D about nine days before maximum, at a redshift consistent with that of its host (NGC 4619 at z = 0.023106, de Vaucouleurs et al. 1991 via NED). | 2006-02-11 08:46:00 | infra-red,optical,ultra-violet,asteroid,supernovae | 2006-02-11 | 08:46:00 | 1,248 | [
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] | 731 |
733 | The Optical Counterpart to XTE J1817-330. | M. A. P. Torres (CfA), D. Steeghs (CfA), P. G. Jonker (SRON/CfA), K. Luhman (Pennsylvania State Univ.), J. E. McClintock (CfA), M. R. Garcia (CfA) | We report the counterpart to the X-ray transient and black hole candidate XTE J1817-330 (ATEL #714).
Our observations consist of a series of 5s and 10s g'-band images obtained with the 6.5m Magellan Clay telescope during 2006 Feb 10 09:23-09:42 UT using the multi-object imaging spectrograph LDSS-3. The frames were acquired with an image quality of 1.2 arcsec and a projected pixel scale of 0.188 arcsec/pixel. The images were calibrated using the Landolt and u'g'i'r' standard star G 162-62 that was observed at similar airmass as XTE J1817-330.
Comparison of our images with the Digitized Sky Survey and 2MASS shows a new single point-like source consistent with the position reported for the radio and near-infrared counterparts (ATEL #721, #724). We measure a mean magnitude for the optical counterpart of g'= 14.93 +/- 0.05 from preliminary photometry.
The optical apparent magnitude is comparable to the K-band magnitude reported in ATEL #724 and supports a low reddening towards the source. The large outburst amplitude in the optical band (the source is not detected in POSS plates) suggests a short orbital period system (see e.g. Shahbaz & Kuulkers,1998,MNRAS,295,L1).
Follow-up observations at all wavelengths, in particular UV, are encouraged. A finding chart for the candidate may be found at: http:/hea-www.cfa.harvard.edu/~mtorres/XTEJ1817m330/ | 2006-02-11 09:57:00 | radio,optical,x-ray,binary,black hole,star,transient,request for observations | 2006-02-11 | 09:57:00 | 1,364 | [
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] | 732 |
734 | Three active neutron star X-ray transients: SAX J1747.0-2853, XTE J1739-285 and GRS 1747-312 | J. Chenevez (DNSC, Denmark), S. E. Shaw (Southampton, UK/ ISDC, Geneva), E. Kuulkers (ESA/ESAC, Spain), S. Brandt, (DNSC, Denmark), T. J.-L. Courvoisier (ISDC, Geneva), K. Ebisawa (NASA/GSFC, USA), P. Kretschmar (ESA/ESAC, Spain), C. Markwardt (NASA/GSFC, USA), N. Mowlavi (ISDC, Geneva), T. Oosterbroek (ESA/ESTEC, Netherlands), A. Orr (ESA/ESTEC, Netherlands), A. Paizis (ISDC, Geneva / IASF, Milano), C. Sanchez-Fernandez (ESA/ESAC, Spain), R. Wijnands (UvA, Netherlands), J. Zurita (ISDC, Geneva) | Apart from the active black-hole candidate X-ray transient XTE J1817-330 (ATel #714), three known neutron star X-ray transients have been found to be active in the INTEGRAL Galactic Bulge monitoring observations on 9 Feb 2006 (ATel #731). These are SAX J1747.0-2853, XTE J1739-285 and GRS 1747-312. The former two were already active near the end of the second period (26 Oct 2005) of our monitoring observations (ATels #615, #622, #642). Since there have been no intermediate INTEGRAL observations of the region in between the two periods, due to sun-angle contraints, we cannot say whether they remained active or whether they showed renewed activity. The latter source (located in Terzan 6) is known to show outbursts roughly every 4.5 months (in 't Zand et al. 2003, A&A 406, 233). Judged from the publicly available RXTE/ASM light curves the last outburst seemed to have indeed occurred in Sep 2005.
SAX J1747.0-2853, XTE 1739-285, and GRS 1747-312 were seen with average JEM-X fluxes of 15 mCrab, 66 mCrab and 35 mCrab in the 3-10 keV band, respectively, and of 15 mCrab, 24 mCrab and 18 mCrab in the 10-25 keV band, respectively. The uncertainty in the JEM-X fluxes in both energy bands is around 1 mCrab. SAX J1747.0-2853 was detected at the 5 sigma level with IBIS/ISGRI with a flux of 8 +/- 2 mCrab, while XTE 1739-285 and GRS 1747-312 were not detected by IBIS/ISGRI with 5 sigma upper limits of typically 10-15 mCrab.
Power-law spectral fits to the JEM-X spectra revealed steep power-law indices with values of ~2.8, ~5.7, and ~4.6, for SAX J1747.0-2853, XTE 1739-285, and GRS 1747-312, respectively. A weak X-ray burst was seen from SAX J147.0-2853 on UTC 11:40, 9 Feb 2006.
Further observations are encouraged. | 2006-02-11 19:59:00 | x-ray,binary,globular cluster,neutron star,star,the sun,transient,variables | 2006-02-11 | 19:59:00 | 1,727 | [
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] | 733 |
735 | Optical classification of 5 Swift hard X-ray sources | N. Masetti, L. Bassani (IASF/INAF, Bologna), A. J. Dean (Univ. Southampton), P. Ubertini (IASF/INAF, Rome) and R. Walter (ISDC, Versoix) | Between February 6 and 10, 2006, we used the instrument BFOSC mounted on the `G.D. Cassini' 1.5m telescope of the Astronomical Observatory of Bologna located in Loiano (Italy) to acquire optical spectra of the counterparts to 5 hard X-ray sources recently discovered by Swift (see ATels #669, #677 and #697) in order to assess their nature. Total exposure times ranged from 40 to 80 minutes, depending on the object brightness.
In the following table, we report the classification and redshift of these 5 sources:
Notes on individual sources.
SWIFT J0444.1+2813: narrow Halpha, Hbeta, [NII], [SII], [OI] and [OIII] emissions on a reddened continuum are detected in the spectrum of the optical counterpart. All features are at redshift z = 0.010+-0.001, consistently with the 21cm radio measurement of Pantoja et al. (1997, AJ, 113, 905). The line narrowness and their ratios indicate that this is a Seyfert 2 galaxy.
SWIFT J0732.5-1331: the Swift/XRT error box encompasses two objects. The brighter one (mag. R ~ 12.5) has the spectrum of a normal G/K type Galactic star. The fainter one (mag. R ~ 14), located ~10 arcsec SE, is the true optical counterpart: spectroscopy reveals Halpha, Hbeta, HeI 5875 and HeII 4686 in emission at redshift zero, superimposed on a very blue and otherwise featureless continuum. These signatures are typical of an accretion disk of a Galactic X-ray binary, most likely a Low Mass X-ray Binary.
SWIFT J0823.4-0457: the optical spectrum of the counterpart, galaxy LEDA 23515, shows narrow Halpha, Hbeta, [NII], [SII], [OI] and [OIII] emission lines over a flat continuum. These features are at redshift z = 0.023+-0.001, consistent with Fouque et al. (1992, Catalogue of optical radial velocities, Obs. Lyon et Paris-Meudon, Vol. 1, p. 1). Here also, the line shapes and ratios indicate that this is a Seyfert 2 galaxy.
SWIFT J0918.5+1618: broad Balmer emissions at least up to Hdelta, as well as narrow Halpha, Hbeta, [NII], [SII], [OI], [OIII], HeI and HeII emission lines are detected in the optical spectrum of the counterpart, which moreover shows a blue continuum. From the observed wavelengths of narrow features, we determine a redshift z = 0.029 +- 0.001. The overall spectral appearance allows us to classify this object as a Seyfert 1 galaxy.
SWIFT J1200.8+0650: here, Halpha, Hbeta, [NII], [SII], and [OIII] narrow emission lines are detected over the relatively flat spectral continuum of the optical counterpart, the galaxy LEDA 37894. The features are at redshift z = 0.035+-0.001, consistently with Grogin et al. (1998, ApJS, 119, 277). The line shape and ratios indicate that this also is a Seyfert 2 galaxy.
We thank R. Gualandi and S. Bernabei for the night assistance at the telescope. | 2006-02-14 00:42:00 | radio,optical,x-ray,agn,binary,star | 2006-02-14 | 00:42:00 | 2,745 | [
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] | 734 |
736 | Supernova Discoveries: Type IIn SNF20060209-002 and Type Ia SNF20060209-003 | The Nearby Supernova Factory: N. Blanc, Y. Copin, E. Gangler, G. Smadja (Institut de Physique Nucleaire de Lyon), P. Antilogus, S. Gilles, R. Pain, R. Pereira (Laboratoire de Physique Nucleaire et de Haute Energies de Paris), G. Aldering, S. Bailey, S. Bongard, D. Kocevski, B. C. Lee, S. Loken, P. Nugent, S. Perlmutter, R. Scalzo, R. C. Thomas, L. Wang, B. A. Weaver (Lawrence Berkeley National Laboratory, Berkeley, CA), E. Pecontal, G. Rigaudier (Centre de Recherche Astronomique de Lyon), R. Kessler (Kavli Institute for Cosmological Physics, Chicago, IL), C. Baltay, D. Rabinowitz, A. Bauer (Yale) | The Nearby Supernova Factory reports the discovery and classification of two supernovae. Both were discovered in images obtained using the QUEST II camera on the Palomar Oschin 48-inch telescope as a part of the JPL Near-Earth Asteroid Tracking component of the Palomar Consortium. Spectra (range 320-1000 nm) of these objects were obtained using the Supernova Integral Field Spectrograph (SNIFS) on the University of Hawaii 2.2-meter telescope for classification purposes.
SNF20060209-002 (coordinates RA 12:00:17.12 DEC +28:36:22.0 J2000.0) was discovered in QUEST II images obtained February 9.4 UT at an approximate magnitude of 17.9 (calibrated to R). A SNIFS spectrum obtained February 15.5 UT reveals it to be a Type IIn supernova at an approximate redshift of z = 0.035, measured from the peak of the H-alpha emission. The continuum is extremely blue, and other Balmer lines are visible.
SNF20060209-003 (coordinates RA 13:46:13.71 DEC -09:07:50.6 J2000.0) was discovered in QUEST II images from February 9.6 UT at an approximate magnitude of 18.6 (calibrated to R). A SNIFS spectrum taken February 15.6 indicates that this is a spectroscopically normal Type Ia supernova about one week past maximum light at an approximate redshift of z = 0.05 as measured by comparison to a library of supernova spectra. | 2006-02-16 07:07:00 | infra-red,optical,ultra-violet,asteroid,supernovae | 2006-02-16 | 07:07:00 | 1,315 | [
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] | 735 |
737 | Strong Hard X-Ray Emission from RS Oph in Outburst | J. L. Sokoloski (SAO), K. Mukai (GSFC), G. J. M. Luna (SAO) | We report on the first X-ray observation of the recurrent nova RS Oph during the 2006 outburst. The Rossi X-ray Timing Explorer (RXTE) observed RS Oph for 1.5 ks on Feb 15, 2006, beginning at 21:43:00 UT. At that time, RS Oph was less than one week into the eruption. A preliminary analysis shows that it was detected out to approximately 25 keV at about 145 counts/s/PCU, with a 2-10 keV flux of (1.33+0.05/-0.01) e-9 erg/cm/cm/s and a 2-20 keV flux of (1.98+0.07/-0.01) e-9 erg/cm/cm/s. Taking a distance of 0.6 kpc (Snijders 1987, in "RS Oph and the Recurrent Nova Phenomenon, ed. M. F. Bode), the absorbed 2-20 keV luminosity is approximately 8.5-8.8 e34 erg/s. An absorbed thermal bremsstrahlung model and an absorbed shock model both give plasma temperatures near 10 keV and an absorbing column of greater than 4e22 cm^-2. The spectrum also contains a strong line at 6.645+/-0.006 keV according to a single Gaussian fit, which may be a blend of several components that are unresolved with the PCA. The plasma temperature of kT=10 keV is consistent with the X-ray emission arising from nebular material that has been shock-heated by ejecta moving at a velocity of around 3000 km/s. The X-ray emission from RS Oph just a few days into this eruption is significantly harder than the X-ray emission detected by EXOSAT during the previous outburst (in 1985) several months after the start of that event (Mason et al. 1987, in "RS Oph and the Recurrent Nova Phenomenon"). | 2006-02-17 01:52:00 | x-ray,binary,cataclysmic variable,nova,star,transient,variables | 2006-02-17 | 01:52:00 | 1,471 | [
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] | 736 |
738 | INTEGRAL and RXTE monitoring of XTE J1817-330: evolving through a state change? | E. Kuulkers (ESA/ESAC, Spain), P. Goldoni (APC & CEA, Saclay), S. E. Shaw (Southampton, UK/ ISDC, Geneva), S. Brandt, J. Chenevez (DNSC, Denmark), T. J.-L. Courvoisier (ISDC, Geneva), K. Ebisawa (NASA/GSFC, USA), P. Kretschmar (ESA/ESAC, Spain), C. Markwardt (NASA/GSFC, USA), N. Mowlavi (ISDC, Geneva), T. Oosterbroek, A. Orr (ESA/ESTEC, Netherlands), A. Paizis (IASF, Milano), J. Rodriguez (CEA, Saclay), C. Sanchez-Fernandez (ESA/ESAC, Spain) & R. Wijnands (UvA, Netherlands) | INTEGRAL Galactic Bulge monitoring observations (ATel #438) indicate that the X-ray transient and black-hole candidate XTE J1817-330 (ATel #714) has increased in hard X-rays (20-60 keV) compared to the observations performed on Feb 9, 2006 (ATel #731). The 20-60 keV fluxes were 46+/-2 mCrab on Feb 11 and 79+/-2 mCrab on Feb 14. The 60-150 keV fluxes did not show a significant increase: they were 45+/-7 and 60+/-7 mCrab, respectively, on the above quoted days. Preliminary spectral analysis indicates that in the range 20-150 keV the spectrum of the source has indeed steepened: a power-law with photon index of 2.6+/-0.1 fits the INTEGRAL observations on Feb 14.
The RXTE/PCA Galactic Bulge scans, however, show a decrease of the source at lower energies (2-10 keV), from 840 mCrab on Feb 9 to 710 mCrab on Feb 12 to 670 mCrab on Feb 15 (all +/-4 mCrab). This is in contrast to the spectral behaviour described above.
These findings may indicate a state change, which could be accompanied by changes in the emission at other wavelengths. We again note that an INTEGRAL ToO observation of XTEJ1817-330 is presently ongoing and will last up to Feb 17, 11:20 UTC. Observations at other wavelengths are therefore encouraged. | 2006-02-17 03:07:00 | x-ray,gamma ray,binary,black hole,transient,variables | 2006-02-17 | 03:07:00 | 1,226 | [
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] | 737 |
739 | Confirmation of counterpart to SWIFT J1626.6-5156 | Ignacio Negueruela, Amparo Marco (University of Alicante) | The candidate counterpart to SWIFT J1626.6-5156 (ATel #678, #679, #688) proposed by Rea et al. (ATel #713) was observed on the night of 2006 Feb 15 with the NTT (La Silla, Chile). The instrument used was EMMI with grism #6. This configuration covers the 570-870 nm range with a dispersion of 0.7A/pixel.
The candidate (2MASS16263652-5156305 = USNO-B1.0 0380-0649488) displays H-alpha strongly in emission, with an EW=-38Ã
and broad wings. The Paschen series is also in emission, with Pa 18 rather stronger than other lines, most likely because of an important contribution from OI 8446Ã
. No HeI lines are seen, though HeI 7065Ã
may be very weakly in emission. Weak emission from the OI 7774Ã
triplet is also possibly detected. Though a blue spectrum will be necessary for an exact classification, all these features strongly suggest that the object is a Be star and hence SWIFT J1626.6-5156 is an unusual Be/X-ray binary. | 2006-02-17 05:02:00 | optical,x-ray,binary,pulsar,star,transient | 2006-02-17 | 05:02:00 | 926 | [
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] | 738 |
740 | Swift-UVOT detection of XTEJ1817-330 in the UV | D. Steeghs, M. A.P. Torres (CfA), J. Miller (UMich), P. G.Jonker (SRON/CfA) | The SWIFT Observatory performed a TOO observation of the active transient XTE J1817-330 (ATel #714) on Feb 18th 2006, covering 04:50-05:10UT. The Ultra-Violet/Optical Telescope (UVOT) collected a series of 160-190s exposures of the field surrounding the transient using its six broad-band filters.
Processed UVOT images reveal a well detected point source at the reported position of the transient (ATel #721,#724,#733) in all filters. The transient is particularly evident in the UV filters. After extracting the source counts, we used the latest UVOT calibration files and derived the following magnitudes and fluxes in the UVOT pass-bands;
Given the sensitivity of the UV flux to interstellar extinction, these fluxes clearly demonstrate the low hydrogen column along the line of sight towards XTE J1817-330. Comparing the above fluxes with hot black-body models suggests a hydrogen column around 2-5 10^21. The ultra-violet constraints permitted thanks to such a modest column will greatly enhance ongoing efforts targeting this bright transient at X-ray wavelengths.
We thank the SWIFT team for their cooperation and encourage observations of this source at all wave-bands. | 2006-02-20 05:14:00 | optical,ultra-violet,x-ray,binary,black hole,neutron star,star,transient | 2006-02-20 | 05:14:00 | 1,181 | [
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741 | Second RXTE Observation of RS Oph in Outburst | J. L. Sokoloski, G. J. M. Luna (SAO), K. Mukai (GSFC) | We report on the second Rossi X-Ray Timing Explorer (RXTE) observation of the symbiotic recurrent nova RS Oph in outburst. This 2.3 ks observation was performed roughly one week into the eruption, on Feb 18, 2006, beginning at 17:27:00 UT. A preliminary analysis indicates that the source is still X-ray bright. We find a 2-10 keV flux of (1.54+/-0.05) e-9 erg/cm/cm/s and a 2-20 keV flux of (1.80+/-0.05) e-9 erg/cm/cm/s. Taking a distance of 1.6 kpc (note the different assumed distance compared to ATel #737; Snijders 1987, in "RS Oph (1985) and the Recurrent Nova Phenomenon", ed. M. F. Bode), the absorbed 2-20 keV luminosity is approximately (5.5+/-0.1) e35 erg/s (compared to (6.0+/-0.1) e35 erg/s on Feb 15). The spectrum softened compared to the first outburst X-ray observation three days earlier (see ATel #737). An absorbed thermal bremsstrahlung model gives a plasma temperature of approximately 5 to 6 keV, compared to approximately 10 keV on Feb 15. The X-ray spectral evolution is thus consistent with shock heating by ejecta that is decelerating. A plasma temperature of 5-6 keV corresponds to a strong shock moving at around 2200 km/s. The complex of Fe lines near 6.6 keV also significantly decreased in strength. Finally, the absorbing column dropped to roughly 5e21 cm^-2, which is close to the interstellar value of 3-4 e21 cm^-2 given by Mason et al. (1987, in "RS Oph (1985) and the Recurrent Nova Phenomenon"). | 2006-02-21 02:11:00 | x-ray,binary,cataclysmic variable,nova,star,transient,variables | 2006-02-21 | 02:11:00 | 1,435 | [
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] | 740 |
742 | INTEGRAL pointed observation of XTEJ1817-330 | P. Goldoni (APC & CEA, Saclay), E. Kuulkers (ESA/ESAC, Spain), J. Rodriguez (CEA, Saclay), S. E. Shaw (Southampton, UK/ ISDC Geneva), P. Dubath (ISDC Geneva), J. Chenevez, N. Lund (DNSC, Copenhagen), A. Goldwurm, M. Cadolle Bel (APC & CEA Saclay), M. Del Santo, P. Ubertini, A. Bazzano (INAF/IASF, Rome), C. Winkler (ESA/ESTEC, Netherlands) | We report preliminary results of the INTEGRAL ToO observation of the transient BHC XTEJ1817-330 (ATEL #714, #731) performed from 2006-02-15 01:28:29 (U.T.C.) to 2006-02-17 11:19:41.0 for a total exposure time of about 200 ksec. The source has been clearly detected up to 200 keV with no apparent cutoff at flux levels of about 1 Crab (3-20 keV) and 90 mCrab (20-200 keV). Preliminary analysis of JEM-X and IBIS/ISGRI data show that the 3-200 keV spectrum of the source can be well fitted by a disk black body with temperature of 0.9 keV plus a powerlaw with photon index 2.7. In agreement with previous reports (ATEL #724, #733, #740), no interstellar absorption was needed in the fit, suggesting a low column density (Nh~10^21 cm^-2). The power density spectrum, computed from the 3-15 keV JEM-X light curve, is consistent with white noise above ~1 mHz, while it is well represented by a power law with index ~2.07 below 1mHz. We estimate the RMS fractional amplitude to be ~6% between 0.01mHz and 1mHz. The relative weakness of the hard component and the low level of variability suggest that the source has been observed predominantly in the high/soft state, although some evolution could be seen. We also searched for signatures of 511 keV emission features in 3 hour-long sections of the SPI data as well as on the entire observation. No emission was detected with 3 sigma upper limits respectively of 2.4e-3 ph/cm^2/s and 7.5e-4 ph/cm^2/s. XTEJ1817-330 will be observed regularly by INTEGRAL in the following weeks by the Galactic Bulge Monitoring Program (ATEL #734, #738). Further observations are encouraged to follow the evolution of this source. | 2006-02-22 01:05:00 | x-ray,gamma ray,binary,black hole,transient | 2006-02-22 | 01:05:00 | 1,656 | [
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] | 741 |
743 | A Pointed RXTE Observation of XTE J1817-330 | J. M. Miller (Michigan), J. Homan (MIT), D. Steeghs (CfA), M. A. P. Torres (CfA), R. Wijnands (Amsterdam) | We report on a pointed RXTE observation of XTE J1817-330, obtained on 2006-02-13 at 08:10:40 UT. After standard screening, the net good time for the PCA was 9.6 ksec, and the net good time for the HEXTE (cluster A) was 3.0 ksec. Joint fits were made to the PCU-2 and HEXTE-A spectra on the 2.8-25.0 keV and 20.0-200.0 keV range, respectively, with XSPEC. For a variety of continuum spectral models, a low column density is implied. Error scans indicate that a column density in the 0.8-5.0 E+21 range (90% confidence limits), though it seems likely that the column density is as low as 2 E+21. This value corresponds well to the weighted average column density given by the N_H HEASARC tool, based on Dickey & Lockman 1990. A phenomenological model consisting of disk blackbody and power-law continuum components and a Gaussian Fe K line component gives kT = 0.89(1) keV, Gamma = 2.20(3), and a line equivalent width of 240(40) eV (90% confidence errors). There is no evidence for a break or cut-off in the power-law. The line appears to be broadened, and the best fit Gaussian centroid energy lies between 5.5-6.0 keV. The source appears to be clearly detected out to 200 keV. The above model gives an unabsorbed flux of 1.3 E-8 erg/cm^2/s in the 3-200 keV band, a flux of 4.6 E-8 erg/cm^2/s in the 0.5-200 keV band, and a flux of 4.4 E-8 erg/cm^2/s in the 0.5-10.0 keV band. The disk contributes 90% of the flux in the 0.5-10 keV band, and 77% of the flux in the 3-200 keV band. These fit parameters and fluxes, and the 1/f nature of the power spectra we have observed, are consistent with the source being in the high/soft (= thermal-dominant) state on February 13. ATEL 738 indicates that the power-law softened after this RXTE observation. Particularly given that the low column density implied in X-rays confirms optical inferences (see ATEL 740, ATEL 733), we strongly encourage joint optical and X-ray follow-up of this source. | 2006-02-22 01:26:00 | optical,ultra-violet,x-ray,binary,black hole,transient | 2006-02-22 | 01:26:00 | 1,935 | [
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] | 742 |
744 | Renewed X-ray activity of IGR J17419-2802 and GRS 1736-297 observed with INTEGRAL | S. A. Grebenev (IKI, Moscow), S. V. Molkov (IKI, Moscow), R. A. Sunyaev (IKI, Moscow; MPA, Garching) | Two X-ray transients, IGR J17419-2802 and GRS 1736-297, were found to be in outburst with the IBIS/ISGRI telescope on board INTEGRAL on February 19-20, 2006, during deep Open Program observations of the Galactic center field.
The first source, IGR J17419-2802, was detected with the signal-to-noise (S/N) ratio 12.2 and the average flux 7.7+/-0.6 mCrab in the 18-45 keV band. This source was discovered by INTEGRAL in September 2005 (ATEL #616), was localized with a few arcsec accuracy by SWIFT/XRT (ATEL #617) but still was not identified.
GRS 1736-297 was detected with the S/N ratio 6.8 and the average flux 4.4+/-0.6 mCrab in the same 18-45 keV band. The source was discovered by the GRANAT/ART-P telescope in September-October 1990 (Pavlinsky et al., SvAL, 1992, 18, 88), detected in the ROSAT all-sky survey (as 1RXS J173930.3-294211) and suspected to be a Be-system by Motch et al. (A&A, 1998, 132, 341). It has not been detected in all subsequent X-ray observations including the pointed observation with Chandra (Wilson et al., ApJ, 2003, 596, 1220).
We encourage follow-up observations of both sources at all wavelengths. | 2006-02-23 02:01:00 | radio,infra-red,optical,x-ray,black hole,neutron star,star,transient,request for observations | 2006-02-23 | 02:01:00 | 1,135 | [
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] | 743 |
745 | Refined X-ray position of IGR J17419-2802 | A. K.H. Kong (MIT) | We reanalyze the Swift XRT observation of IGR J17419-2802 taken on 2005 October 3 (ATel #617) and obtain a refined X-ray position of the source. The source is located at R.A. = 17h41m56.0s, Dec = -28:01:54.5 (J2000) with an estimated uncertainty of 3.6 arcsec (90% confidence radius). This position includes the latest XRT boresight correction. The refined position is 5.5 arcsec from the previous XRT position (ATel #617). We note that one 2MASS object with K=12.2 is within the refined error circle. | 2006-02-23 05:30:00 | x-ray,transient | 2006-02-23 | 05:30:00 | 501 | [
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] | 744 |
746 | Chandra Constraints on the Column Density to XTE J1817-330 | J. M. Miller (Michigan), J. Homan (MIT), D. Steeghs (CfA), R. Wijnands (Amsterdam) | We observed the black hole candidate with Chandra for 50 ksec, starting on Feb 13 2006 at 02:04 UT. The HETGS was used to obtain a high resolution spectrum, which was read-out with the ACIS-S array. Initial fits to the spectra have been made using XSPEC and ISIS. For a number of continuum models, and neutral absorption models, we find N_H = 8.8-9.7 E+20 cm^-2. This value is even lower than that anticipated in ATEL 743. The continuum spectrum is dominated by a kT = 0.93 keV disk, throughout the 0.5-10.0 keV band. Our results indicate that the column density along the line of sight to XTE J1817-330 is lower than all strong black hole candidates, apart from XTE J1118+480. We strongly urge efforts to coordinate fast X-ray and optical photometry to search for simultaneous QPOs. | 2006-02-24 01:01:00 | optical,x-ray,binary,black hole,transient | 2006-02-24 | 01:01:00 | 783 | [
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] | 745 |
747 | Third RXTE Observation of RS Oph in Outburst: Beginning of the X-ray Decline | J. L. Sokoloski, G. J. M. Luna (SAO), K. Mukai (GSFC) | We report on the third Rossi X-Ray Timing Explorer (RXTE) observation of the symbiotic recurrent nova RS Oph in outburst. A preliminary analysis of this 1.56 ks observation, performed on Feb 22.60 UT (approximately 10 days after optical maximum), reveals that the source is continuing to soften in the X-rays, and that it has started to fade. We find a 2-10 keV flux of (7.10+/-0.05) e-10 erg/cm/cm/s and a 2-20 keV flux of (7.72+/-0.05) e-10 erg/cm/cm/s. These fluxes are down by more than a factor of 2 compared to the previous RXTE observation of RS Oph, performed 4 days earlier (see ATel #741). Taking a distance of 1.6 kpc, the absorbed 2-20 keV luminosity is (2.4+/-0.1) e35 erg/s. The hard X-ray spectrum can be roughly characterized by thermal emission from a plasma with kT = 4 keV (compared to a plasma temperature of near 10 keV approximately 3 days after optical maximum and 5 to 6 keV approximately 6 days after optical maximum). The Fe line complex near 6.6 keV has continued to decrease in strength, with its equivalent width going from just over 1 keV in the first two RXTE observations to roughly 0.7 keV on Feb 22. Although the RXTE data do not place strong constraints on the column density, the spectrum is consistent with absorption solely from the interstellar medium. | 2006-02-24 10:24:00 | optical,x-ray,binary,cataclysmic variable,nova,star,transient,variables | 2006-02-24 | 10:24:00 | 1,291 | [
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] | 746 |
748 | Spectral evolution and kHz QPOs in the transient Z source XTE J1701-462 | Jeroen Homan (MIT), Tomaso Belloni (INAF/OAB), Michiel van der Klis, Piergiorgio Casella (U. Amsterdam), Mariano Mendez (SRON), Walter Lewin (MIT), Rob Fender (U. Southampton), Elena Gallo (UCSB), and Neil Gehrels (NASA/GSFC) | Since our last report on the transient Z source XTE J1701-462 (ATel #725), RXTE has continued observing the source on an almost daily basis. Spectral evolution similar to that reported by Homan et al. (ATel #725) is being observed, albeit at progressively lower luminosities, suggesting that the source has begun its decay. By following the count rate of a fixed location along the 'Z-track' (we chose the middle of the normal branch) we estimate that the luminosity has decreased by a factor of two since maximum. In addition to the lower luminosities the overall shapes in the color-color and color-intensity diagrams seem to be evolving and moving to harder colors. In particular, the upturn in the horizontal branch and the dips observed in the flaring branch are no longer observed. This suggests that the source might be evolving from a 'Cyg X-2 like' Z source to a 'Sco X-1 like' Z source (see Kuulkers et al. 1994, A&A, 289, 795 for a discussion).
Lately, the source has spent a relatively large fraction of its time on the normal and flaring branches. During one brief excursion onto the horizontal branch we saw strong indications for twin kHz QPOs at 651 Hz and 908 Hz. Although these detections are only a little more significant than 3 sigma (single trial), it should be noted that their frequencies fall right on top of well established frequency-frequency relations for similar pairs of kHz QPO in other neutron star LMXBs.
Finally, the broad bump in the power spectrum around 6 Hz that we tentatively identified as the normal-branch QPO (ATel #725) has evolved into a narrower feature, just like the normal-branch QPO seen in other Z sources.
More RXTE observations have been planned. | 2006-02-25 04:59:00 | x-ray,binary,neutron star,star,transient | 2006-02-25 | 04:59:00 | 1,703 | [
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] | 747 |
749 | Optical Spectroscopy of XTE J1817-330 in Outburst | M. A.P. Torres, D. Steeghs, J. McClintock, M. Garcia (CfA), Alexis Brandeker, Duy Nguyen (Toronto), P. G.Jonker (SRON/CfA), J. M.Miller (Michigan) | A single 30 min high-resolution spectrum of the optical counterpart to the black hole candidate XTE J1817-330 (ATEL #714, #733) was acquired with the MIKE echelle spectrograph on the Magellan-Clay telescope at Las Campanas Observatory on Feb 20 2006 08:36 UT. In the blue (red), MIKE covered the wavelength range 3530-5070 (4830-9420) Angstrom with a dispersion varying between 0.03 and 0.05 (0.07 and 0.013) A/pix.
The only emission line detected in the spectrum is Halpha with equivalent width (EW) of ~ 4 A and FWHM ~ 640 km/s. No other Balmer lines (in emission/absorption) were detected, nor was there evidence for HeII 4686 A or Bowen blend emission. The signal-to-noise ratio was ~40-45 at Hbeta, Hgamma and HeII.
We clearly detect the CaII H&K and the NaD interstellar lines in absorption, but we do not find absorption line features that would be expected from a local absorber. The EW of the NaD 5890,5996 A components were measured to be 0.68 +/- 0.04 A and 0.48 +/- 0.04 A respectively. The EW uncertainties were estimated by looking at the scatter in the values when selecting different wavelength intervals to reflect the local continuum level.
The ratio between the two Sodium lines is much less than the factor of two expected at the lowest optical depths (Munari & Zwitter 1997,A&A,318,269). The total EW of the doublet corresponds to E(B-V) = 0.29 +/- 0.01 mag according to the empirical relationship of Barbon et al. (1990,A&A,237,79). However, the calibration of Munari & Zwitter (1997) would yield a much higher extinction of E(B-V) > 0.7 mag. For comparison, the Hydrogen column as estimated from the Schlegel dust maps gives E(B-V)=0.24.
We surveyed the MIKE spectrum to identify other possible interstellar lines (IS) and diffuse interstellar bands (DIBs) that could be used to estimate the reddening using the list of Jenniskens & Desert (1994,A&AS,106,39). We were able to identify the DIB at 5870 A and KI 7699 A with EWs of 0.18 +/- 0.04 A and 0.08 +/- 0.03 A, yielding E(B-V)= 0.44 +/- 0.11 and 0.3 +/- 0.2 respectively when using the calibrations from Herbig (1993,ApJ,407,142) and Munari & Zwitter (1997).
The above estimates indicate that significant differences exist between the various EW versus N_H calibrations. This is the limiting factor in determining the N_H from the MIKE spectrum. We therefore constrain the Hydrogen column to be in the range 1e21 < N_H < 3e21.
These estimates for N_H, together with the independent constraint from the Chandra observations (ATEL #746), confirm that the column towards XTE J1817-330 is modest. | 2006-02-26 06:50:00 | optical,binary,black hole,transient | 2006-02-26 | 06:50:00 | 2,576 | [
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] | 748 |
750 | Radio Observations of RS Oph: Past the First Peak? | G. G. Pooley (MRAO Cambridge), J. L. Sokoloski (CfA), M. P. Rupen, A. J. Mioduszewski (NRAO) | Radio observations of the symbiotic recurrent nova RS Oph made with the Ryle Telescope at Cambridge at 15.2 GHz give the following:
This is a low elevation source for the Ryle Telescope, and these flux densities are correspondingly uncertain, at about the 15% level. Still it seems clear that RS Oph has brightened considerably since the VLA measurement on Feb. 17.5 (23.2 +/- 0.6 mJy at 15 GHz; Eyres et al., IAU Circular 8678), consistent with the 6 GHz rise seen with MERLIN (ibid). The source is clearly not continuing to brighten at the same rate, and may be past its first peak. Further observations are on-going.
The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. | 2006-02-27 23:50:00 | radio,binary,cataclysmic variable,nova,star,transient,variables | 2006-02-27 | 23:50:00 | 781 | [
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] | 749 |
751 | Chandra Observation of Supernova 2006X in M100 | S. Immler, NASA Goddard Space Flight Center, Universities Space Research Association | No X-ray source is detected at the position of the Type Ia SN 2006X in M100 (IAUC # 8667 , CBET #393, ATel #726) in a 37.9 ks Chandra ACIS-S X-ray observation from 2006-02-18.72UT. The 3-sigma upper limit to the (0.2-10 keV band) count rate is 4.5E-04 cts/s, corresponding to an unabsorbed X-ray flux and luminosity of 4E-15 ergs/cm/cm/s and 1E38 ergs/s, respectively, for an assumed thermal plasma spectrum with a temperature of 10 keV, an absorbing foreground column density of 2.39E20 cm**-2 (Dickey & Lockman 1990, ARAA 28, 215) and a distance of 17.1 Mpc (Freedman et al. 1994, Nature 371, 757). The inferred upper limit to the mass-loss rate of the pre-SN system is a few x E-6 M_sun/year assuming a shock velocity of 20,000 km/s and a stellar wind speed of 10 km/s. | 2006-02-28 04:26:00 | x-ray,supernovae,the sun | 2006-02-28 | 04:26:00 | 772 | [
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] | 750 |
752 | Rapid evolution of variability properties in XTE J1817-330 | Jeroen Homan (MIT), Jon M. Miller (Michigan), Rudy Wijnands (Amsterdam) | We observed the black hole candidate X-ray transient XTE J1817-330 five times with RXTE on February 24, between 06:03 UTC and 17:04 UTC. The unabsorbed 4-25 keV fluxes were close to 6.2e-10 ergs/cm^2/s in all five observations, only slightly higher than in our observation of February 13 (ATel #743). However, the 10-25 keV fluxes were more than 2-2.5 times higher in our latest observations, confirming the recent spectral hardening reported in ATel #738. The 4-10 keV fluxes were ~10-20% lower.
During the ~13 hours of observations we observed a remarkably rapid evolution of the variability properties of the source. The power spectra of the first two observations (06:03-08:00 UTC) showed band-limited noise with a QPO around 8.5 Hz. The rms variability in the 0.01-50 Hz range was ~11.5% (6-60 keV). The third observation (13:20-13:43 UTC) showed 1/f noise with a weak QPO around 6.4 Hz. The strength of the overall variability was only 2.6% rms. In the last two observations (UTC 14:55-17:04) the weak QPO was replaced by a more coherent and stronger QPO around 5.0 Hz, resulting in an increase in the overall variability to ~8% rms. Based on properties such as strength, Q-value, and frequency, we identify the QPOs in observations 1/2, 3, 4/5 as type C, type A, and type B, respectively (see Remillard et al. 2002, ApJ 564, 962 for a definition of these three QPO types in black hole X-ray binaries).
Plots of the power spectra can be found at http://tahti.mit.edu/1817/atel
The changes in the variability properties coincided with subtle changes in the spectral power-law index. For observations 1/2, 3, and 4/5 we measured indices of, 2.32+/-0.02, 2.41+/-0.03, and 2.44+/-0.02, using a similar spectral model as in ATel #743. The 10-25 keV flux varied by 15% between the observations, being the highest in the first two observations, and the lowest in the third. These observations show that significant changes in the variability properties do not necessarily require large spectra changes (at least not in the RXTE/PCA energy band).
Finally, we note that the sudden changes we observed in the power spectral properties (i.e. noise changing from band-limited to 1/f and QPOs from type C to type A/B) have previously been associated with relativistic jet/ejection events in the radio (see Fender et al. MNRAS, 355, 1105). | 2006-02-28 22:33:00 | radio,x-ray,binary,black hole,transient | 2006-02-28 | 22:33:00 | 2,335 | [
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753 | Swift/XRT detection of a transient source in the Galactic Center | J. A. Kennea (PSU), D. N. Burrows (PSU), S. Campana (OAB), O. Godet (U Leicester), J. Nousek (PSU) and N. Gehrels (GSFC) | We report the detection in late February 2006 of a variable X-ray source near Sgr A*, by the Swift X-Ray Telescope (XRT) in a series of short (~1ks per day) observations of the Galactic Center. We have analyzed data from four observations and detect a bright point source, Swift J174535.5-290135.6, 90 arcseconds from Sgr A*, at the following coordinates: RA = 17h 45m 35.5s, Dec = -29d 01m 35.6s (J2000) with an estimated uncertainty of 6 arcseconds radius (90% containment). We note that source location is 2.8 arcseconds from the Chandra discovered Galactic Center source, CXOGC J174535.6-290133 (Muno et al, 2004). This location is also 4.6 arcseconds from the position of an ASCA detected eclipsing X-ray burster with an ~8.4 hour period, AX J1745.6-2901 (Maeda et al., 1996, Kennea and Skinner, 1996). This source was not detected during a 1025s observation starting on February 24th at 22:55UT, but is the brightest source within 10 arcmin of Sgr A* in a 900s observation 9.6 hours later with a flux of 2.3 x 10^-11 erg/s/cm^2 (0.2-10 keV). The 3 sigma upper limit on the flux in the initial observation is 2 x 10^-13 erg/s (0.2-10 keV). It has a power-law spectrum (photon index ~1.6) and its high absorption (1.4 x 10^23 cm^-2) suggesting it is located at the Galactic Center. Assuming a distance of 8.5 kpc, the X-ray luminosity of this source is approximately 3 x 10^35 erg/s (0.2-10 keV), corrected for absorption. In 2 further observations starting on February 26th at 08:40UT and February 27 at 07:11UT the source remains on, fading gradually with a power-law slope of approximately -0.15. As we have no observations of this field prior to February 24th, we cannot determine if the non-detection of this source on that day was due to the source being in eclipse, or if the source was in a low flux state prior to the February 25th detection. If the source is AX J1746.7-2901, the eclipse hypotheses for the non-detection of the source is unlikely as Maeda et al. (1996) report the flux during eclipse is ~20% of the un-eclipsed level, which would have been detected in our observation. We note that the spectral parameters for CXOGC J174535.6-290133 are consistent with Swift J174535.5-290135.6, however the reported absorbed flux is ~1000 times fainter than the Swift/XRT detected flux. AX J1745.6-2901 has been shown to vary in brightness over long time periods (e.g. Sakano et al., 2002), and we tentatively suggest that the Swift source may be AX J1745.6-2901 re-entering a high state. Observations of this source are on-going. | 2006-03-01 02:59:00 | x-ray,transient,variables | 2006-03-01 | 02:59:00 | 2,545 | [
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754 | Fourth RXTE Observation of RS Oph in Outburst: Continued Fading | J. L. Sokoloski, G. J. M. Luna (SAO), K. Mukai (GSFC) | We report on the fourth Rossi X-Ray Timing Explorer (RXTE) observation of the symbiotic recurrent nova RS Oph in outburst. A preliminary analysis of this 3.42 ks observation, performed on Feb 26.87 UT (approximately 14 days after optical maximum), reveals that the source is continuing to both soften and fade in the hard X-rays. We find a 2-10 keV flux of (3.48+0.02/-0.11) e-10 erg/cm/cm/s and a 2-20 keV flux of (3.59+/-0.1) e-10 erg/cm/cm/s. The fluxes have dropped by about a factor of 2 in four days, as they did between Feb 18 and Feb 22 (outburst days 6 and 10; see ATel #741 and ATel #747). Taking a distance of 1.6 kpc, the absorbed 2-20 keV luminosity is (1.1+/-0.05) e35 erg/s. The absorbed 2-20 keV luminosity has fallen from a peak value of (6.0+/-0.1) e35 erg/s 3 days after optical maximum (see ATel #737). The hard X-ray spectrum can be roughly characterized by thermal emission from a plasma with kT = 2.8 keV. The equivalent width of the Fe complex near 6.6 keV is now less than 0.7 keV. Although the RXTE data do not place strong constraints on the column density, the spectrum is consistent with absorption solely from the interstellar medium. | 2006-03-01 06:19:00 | optical,x-ray,binary,cataclysmic variable,nova,star,transient,variables | 2006-03-01 | 06:19:00 | 1,164 | [
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] | 753 |
755 | No Radio Emission from IGR J17419-2802 or GRS 1736-297 | M. P. Rupen, A. J. Mioduszewski, V. Dhawan (NRAO) | Pursuant to the report of renewed X-ray activity in IGR J17419-2802 and GRS 1736-297 (ATel #744) on Feb. 19-20, both sources were observed with the Very Large Array (VLA) at 4.86 GHz on Feb. 26. In the case of IGR J17419-2802, there was no source within the revised Swift XRT error circle (ATel #745) with an rms of 95 microJy/beam; the min/max within that error circle were (-0.37, +0.32) mJy/beam. In the case of GRS 1736-297, there was no source within the 90 arcsecond GRS error circle (Pavlinksy et al. 1994 ApJ 425, 110; Cherepashchuk et al. 1994 A&A 289, 419), with an rms noise of 99 microJy/beam. Although the min/max within the latter error circle were +/-0.49 mJy/beam, bandwidth smearing in these high-resolution (A configuration) continuum observations leads to a more realistic limit of perhaps 1 mJy/beam on any radio emission.
We also observed IGR J17419-2802 in October 2005, with no detections. On Oct. 9th, the nominal flux density at the Swift location was 0.016 +/- 0.071 mJy/beam, at 8.46 GHz; on Oct. 10th, the nominal flux density was 0.034 +/- 0.099 mJy/beam, at 4.86 GHz. We note that the Swift X-ray detection (ATel #617) was made on Oct. 3rd, 2005.
The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. | 2006-03-02 06:17:00 | radio,x-ray,black hole,neutron star,star,transient | 2006-03-02 | 06:17:00 | 1,338 | [
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756 | INTEGRAL detects SWIFT J174535.5-290135.6 | J. Chenevez (DNSC, Denmark), C. Sanchez-Fernandez (ESA/ESAC, Spain), E. Kuulkers (ESA/ESAC, Spain), S. Shaw (Southampton, UK/ ISDC, Switzerland), S. Brandt (DNSC, Denmark), T. J.-L. Courvoisier (ISDC, Switzerland), K. Ebisawa (NASA/GSFC, USA), P. Kretschmar (ESA/ESAC, Spain), C. Markwardt (NASA/GSFC, USA), N. Mowlavi (ISDC, Switzerland), T. Oosterbroek, A. Orr (ESA/ESTEC, Netherlands), A. Paizis (IASF, Milano), R. Wijnands (UvA, Netherlands) | We report on a detection of the new source SWIFT J174535.5-290135.6 (ATel #753) by the JEM-X monitor during INTEGRAL Galactic Bulge monitoring observations taken between 2006, 17 Feb 21:11 and 18 Feb 00:53 UTC (comprising ~10ks), i.e., a week earlier than the SWIFT detection. At that time the average JEM-X flux was 9 mCrab (+/-1 mCrab) in the 6-10 keV band. The average flux measured by ISGRI was near the detection level, i.e., about 6 mCrab (20-60 keV). The derived JEM-X position (RA= 17h 45m 39s, Dec= -29d 01m 44s) is 47 arcsec from the SWIFT position, which is well inside our uncertainty radius of ~2 arcmin.
The source was not detected above an estimated upper limit of ~7 mCrab (6-10 keV) either during previous Galactic Bulge observations performed on Feb 9, Feb 11/12, and Feb 14/15, or during further Galactic Bulge observations performed on Feb 20/21, Feb 24, and Feb 27 Feb. This is in agreement with the flux measured by SWIFT at ~0.7mCrab (0.2-10 keV) on Feb 25, and suggests that the source flux was gradually decreasing. | 2006-03-03 06:38:00 | x-ray,binary,transient,variables | 2006-03-03 | 06:38:00 | 1,041 | [
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757 | Periodic Optical Signal(s) from Swift J0732.5-1331 | J. Patterson, J. Halpern (Columbia U.), N. Mirabal (U. Michigan), Grant Christie (CBA-Auckland), Jennie McCormick (Farm Cove Observatory), Robert Rea (CBA-Nelson), David Messier (CBA-Connecticut) | On 2006 February 17, we obtained low-resolution spectra on the MDM 2.4m telescope of the proposed optical counterpart of the hard X-ray source Swift J0732.5-1331 (Ajello et al., ATel #697). The optical position is 07h 32m 37.64s, -13° 31' 09.0" (J2000.0). The spectrum looks essentially like that of a normal G star, except for very weak He II 4686 emission that is variable on a time scale of 1 hour. This differs from the description of the spectrum obtained by Masetti et al. (ATel #735) just a few days earlier (H, He I, and He II emission lines, featureless blue continuum).
During February 15-28, time-series photometry was obtained using the small-telescope network of the Center for Backyard Astrophysics (CBA). Nightly light curves were nearly flat, but power-spectrum analysis showed a stable pulsation with a period of 512.42(3) seconds, with most of the power in the first harmonic. This fast, stable period, in conjunction with hard X-rays and Lx/Lopt ~ 1, is the defining signature of the intermediate polars (DQ Herculis stars).
While the pulse period is not in doubt, we continue to puzzle over the orbital period of this (probable) cataclysmic variable. Its 4000-7000 Ã
light is evidently dominated by the secondary, so periodic tidal distortion of a Roche-lobe-filling secondary should be quite easy to see in the light curve. But the upper limit on any signal near a plausible orbital frequency is severe (0.024 mag semiamplitude), and this casts some doubt on our interpretation. A weak candidate signal at 11.3 hours could signify the orbital period, but it requires that the binary be close to face-on (i < 15°). | 2006-03-03 08:37:00 | optical,x-ray,binary,cataclysmic variable,star,variables | 2006-03-03 | 08:37:00 | 1,639 | [
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] | 756 |
758 | Radio imaging campaign on newly-detected jets in GRS1915+105 | J. C.A. Miller-Jones (Univ. of Amsterdam), M. P. Rupen (NRAO), S. A. Trushkin (SAO RAS), G. G. Pooley (MRAO), R. P. Fender (Univ. of Southampton) | We report the detection of a large-scale radio jet in the black hole X-ray binary GRS 1915+105 following an X-ray and radio outburst, and announce the start of an intensive radio imaging campaign.
Daily observations with the RATAN-600 radio telescope showed a major radio flare in GRS 1915+105, peaking at ~350 mJy at 2.3 GHz on Feb. 23rd, 2006. X-ray measurements by the RXTE ASM, combined with radio monitoring with the RATAN-600 and the Ryle Telescope, suggest the outburst began at most a day before this. In response to the RATAN-600 report we have begun a series of radio imaging observations with the Very Large Array (VLA), the Very Long Baseline Array (VLBA), and the Multi-Element Radio-Linked Interferometer Network (MERLIN). Here we report the results of the first two 43 GHz VLA observations, taken on Feb. 24th and 28th.
Extended emission was detected on Feb. 24th. This emission was reasonably well fit by two point sources, the brightest one (18.0 +/- 0.7 mJy) at a position consistent with that of the core (V. Dhawan, priv. comm.), and a second component to the southeast, with a flux density of 5.3 +/- 0.7 mJy. The separation of the two components was 45.4 +/- 2.2 milliarcseconds [mas], at a position angle of 140.4 +/- 2.7 degrees, in good agreement with previous observations of the orientation of the radio jets in this source (e.g., Mirabel & Rodriguez 1994, Nature, 371, 46-48; Fender et al. 1999, MNRAS 304, 865-876). Assuming no contamination by the receding (northern) jet, and taking the proper motion of the approaching component to be the same as that reported by Fender et al. (23.6 +/- 0.5 mas/day), the implied ejection date is Feb. 22nd, consistent with the X-ray and radio light curves.
By the time of the second observation on Feb. 28th, the source had faded markedly, with an integrated flux density of only 3.7 +/- 0.9 mJy at 43 GHz. The approaching (southeastern) component had faded below detectability, although there appeared to be a hint of extension to the NW of the core position, possibly corresponding to the receding jet.
Weekly observations with the VLA will continue through mid-May; VLBA observations were taken on Feb. 28th, and are scheduled for Mar. 4th, 6th, and 9th; MERLIN has also made one observation. The combination should give the best imaging sequence yet on this source, probing the evolving morphology over three orders of magnitude in angular scale. Daily radio monitoring with the RATAN-600 and the Ryle Telescope is on-going, and we encourage parallel observations at other wavelengths.
The results of this radio campaign, including contour plots of the two observations detailed above, may be found at http://remote.science.uva.nl/~jmiller/grs1915/monitoring.html which we plan to update weekly.
The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. | 2006-03-03 20:56:00 | radio,x-ray,binary,black hole,transient,variables | 2006-03-03 | 20:56:00 | 2,932 | [
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] | 757 |
759 | Classification of SNe 2006aq, 2006ar, and SNF20060224-026 | The Nearby Supernova Factory: N. Blanc, Y. Copin, E. Gangler, G. Smadja (Institut de Physique Nucleaire de Lyon), P. Antilogus, S. Gilles, R. Pain, R. Pereira (Laboratoire de Physique Nucleaire et de Haute Energies de Paris), G. Aldering, S. Bailey, S. Bongard, D. Kocevski, B. C. Lee, S. Loken, P. Nugent, S. Perlmutter, R. Scalzo, R. C. Thomas, L. Wang, B. A. Weaver (Lawrence Berkeley National Laboratory, Berkeley, CA), E. Pecontal, G. Rigaudier (Centre de Recherche Astronomique de Lyon), R. Kessler (Kavli Institute for Cosmological Physics, Chicago, IL), C. Baltay, D. Rabinowitz, A. Bauer (Yale) | The Nearby Supernova Factory reports that spectra (range 320-1000 nm) of supernovae 2006aq (in MCG +07-24-32, CBET 419) and 2006ar (in MCG +11-13-36, CBET 420), obtained March 07.6 and 07.5 UT (respectively) with the Supernova Integral Field Spectrograph on the University of Hawaii 2.2-meter telescope, show that SN 2006aq is of Type II and SN 2006ar is of Type Ia. The spectrum of SN 2006aq is similar to that of the Type IIb SN 1993J at an approximate redshift of z = 0.05. The SN appears to have faded rapidly relative to the reported discovery magnitude. SN 2006ar is before or near maximum, with a continuum somewhat redder than normally observed in Type Ia supernovae at this phase.
The Nearby Supernova Factory also reports the discovery of supernova SNF20060224-026 (coordinates RA 13:51:24.88 DEC -11:15:26.8 J2000.0) in images obtained February 24.5 UT at an approximate magnitude of 19.9 (calibrated to R) using the QUEST II camera on the Palomar Oschin 48-inch telescope as a part of the JPL Near-Earth Asteroid Tracking component of the Palomar-QUEST Consortium. A SNIFS spectrum obtained March 07.7 UT reveals that this supernova is of Type Ia, similar to SN 1990N about three weeks past maximum light, at a redshift of z = 0.1. | 2006-03-08 14:13:00 | infra-red,optical,ultra-violet,asteroid,supernovae | 2006-03-08 | 14:13:00 | 1,244 | [
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] | 758 |
760 | Optical identification of Swift J0732.5-1331 | T. Marsh (Warwick), S. Littlefair (Sheffield), V. Dhillon (Sheffield) | On 7 March 2006 we looked at the proposed optical counterpart of the hard X-ray source Swift J0732.5-1331 (Atel #697, #735, #757) using the high-speed multi-band CCD camera ULTRACAM mounted on the 4.2m William Herschel Telescope. This star is a suspected intermediate polar. We detected the pulsations previously reported in Atel #757. However, we also found that the proposed counterpart resolves into two stars approximately 1.8" apart and lying along a North-East/South-West axis. The pulsating source is the North-East star of the pair and was approximately half as bright as its companion in g', but equally bright in u'. The source confusion probably explains the puzzling reports of domination by a G star without any ellipsoidal variations and changes in its optical spectrum (Atel #735 and #757). The G star is presumably the South-West star of the pair and is nothing to do with the X-ray source. | 2006-03-09 03:38:00 | optical,x-ray,cataclysmic variable,star,variables | 2006-03-09 | 03:38:00 | 906 | [
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] | 759 |
761 | SWIFT observation of SN 2006at | P. J. Brown, Pennsylvania State University, and S. Immler, Goddard Space Flight Center, NASA, and Universities Space Research Association, on behalf of the Swift-satellite team | We report on Swift Ultraviolet/Optical Telescope (UVOT) and X-Ray Telescope (XRT) observations of SN 2006at (Dintinjana & Mikuz 2006 CBET #434) obtained on 2006-3-10.63 UT.
UVOT magnitudes are V = 17.5 ± 0.2, B = 18.0 ± 0.3, U = 16.7 ± 0.2, UVW1 [181-321 nm] = 17.1 ± 0.2, UVM2 [166-268 nm] = 17.6 ± 0.2, and UVW2 [112-264 nm] = 17.8 ± 0.2. The blue continuum reported by Yamaoka, Naito & Tokimasa (2006 CBET #434) continues into the UV. Comparing the U-B and B-V colors with other SNe from Poznanski et al. (2002, PASP, 114, 833), the U-B color is about one magnitude bluer than observed in the displayed SNe. The UV colors are much bluer than SNe Ia observed with Swift UVOT but comparable to early observations of the type II-P SN2005cs (Brown et al. in prep.).
No X-ray source is detected at the position of SN 2006at in a simultaneous 1,480 s XRT observation. The 3-sigma upper limit to the count rate is 6.2E-03 cts/s, corresponding to an unabsorbed (0.2-10 keV) X-ray flux of 3.3E-13 ergs/cm/cm/s for an assumed thermal plasma spectrum with a temperature of 10 keV and an absorbing foreground column density of 1.87E+20 cm**-2 (Dickey & Lockman 1990, ARAA 28, 215).
Further Swift observations are scheduled. | 2006-03-11 14:31:00 | optical,ultra-violet,x-ray,supernovae | 2006-03-11 | 14:31:00 | 1,223 | [
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762 | Classification of SN 2006au, a Type II Supernova | The Nearby Supernova Factory: N. Blanc, Y. Copin, E. Gangler, G. Smadja (Institut de Physique Nucleaire de Lyon), P. Antilogus, S. Gilles, R. Pain, R. Pereira (Laboratoire de Physique Nucleaire et de Haute Energies de Paris), G. Aldering, S. Bailey, S. Bongard, D. Kocevski, S. Loken, P. Nugent, S. Perlmutter, R. Scalzo, R. C. Thomas, L. Wang, B. A. Weaver (Lawrence Berkeley National Laboratory, Berkeley, CA), E. Pecontal, G. Rigaudier (Centre de Recherche Astronomique de Lyon), R. Kessler (Kavli Institute for Cosmological Physics, Chicago, IL), C. Baltay, D. Rabinowitz, A. Bauer (Yale) | The Nearby Supernova Factory reports that a spectrum (range 320-1000 nm) of SN 2006au (CBET #426) obtained under bad seeing conditions on March 13.6 UT with the Supernova Integral Field Spectrograph on the University of Hawaii 2.2-meter telescope, shows it to be a Type II supernova at an approximate redshift of z = 0.01, consistent with that of the host (UGC 11057, z = 0.009580, Theureau et al. 1998, A&AS, 130, 333 via NED). Our spectrum shows a well-developed H-alpha P Cygni profile. | 2006-03-13 03:07:00 | infra-red,optical,ultra-violet,supernovae | 2006-03-13 | 03:07:00 | 489 | [
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763 | Optical Spectroscopy of Swift J0732.5-1331 | M. A. P. Torres, D. Steeghs, M. R. Garcia, J. E. McClintock, P. Berlind, P. Zhao, M. Calkins (CfA), P. G. Jonker (SRON/CfA), P. J. Callanan (UCC), T. Marsh, B. T. Gaensicke (Warwick), P. Rodriguez-Gil (IAC), S. Littlefair, V. Dhillon (Sheffield) | In response to the detection of the X-ray source Swift J0732.5-1331 (ATEL #697, #735, #757, #760), we observed its optical counterpart with the Mt. Hopkins 1.5m telescope equipped with the FAST spectrograph. A total of 22 spectra covering 3480-7410 A were acquired between Jan 22 and Mar 1. A 3" slit provided 6 A FWHM resolution. In addition, on March 5 we acquired 2.3 hours of spectroscopy (14 spectra) with the 600 gpm grating and a 2 arcsec slit width (4490-4895 A; 2.4 A FWHM). Exposure times were typically 600s and both J0732.5 and the nearby field star at 1.8 arcsec separation (ATEL #760) were in the slit. However, we do not resolve them.
We extracted the spectra using standard IRAF tasks. In order to obtain a less contaminated optical spectrum of J0732.5, the apertures were edited for each spectrum obtained with the 300 gpm grating, centered and sized interactively in order to obtain a Halpha profile in pure emission and therefore maximize the contribution from the object. The resultant spectra show the Balmer lines in emission from Halpha (FWHM = 22 +/- 1 A) to at least Hgamma; HeII 4686 A (FWHM = 16 +/- 1 A); HeI 5876,6678 A and (maybe) the Bowen blend in emission. The line widths were measured from the average of the 22 spectra. The strength of HeII 4686 A to Hbeta is ~ 2.0, indicating the presence of a strong source of ionising photons, typical of either magnetic CVs or novalike variables. The absorption features are totally due to background contamination from the neighbouring star (we do not have the signal-to-noise to discern absorption lines in J0732.5 itself). Our analysis thus confirms that the strong absorption line features reported in ATEL #757 are due to the nearby field star, and that the spectrum of J0732.5 is consistent with that of a magnetic CV.
The HeII radial velocities suggest a variation with an amplitude of 130 - 200 km/s. For comparison, the velocity errors obtained from the scatter of the measured velocities in the absorption spectrum of the contaminating star are about 30 km/s and 4 km/s for the 300 gpm and 600 gpm grating respectively. We were not able to determine an orbital period from our current data.
The high-excitation emission lines reported here, together with the strong hard X-ray emission (ATEL #697) and stable optical pulsations in the J0732.5 light curve (ATEL #757,#760) support an intermediate polar nature for the source. We encourage further observations to establish the orbital period and other key characteristics. | 2006-03-14 03:28:00 | optical,x-ray,binary,cataclysmic variable,star,variables | 2006-03-14 | 03:28:00 | 2,508 | [
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] | 762 |
764 | The decline and rise of the X-ray flux of RS Oph | J Osborne, K Page, A Beardmore (Leicester), M Bode (Liverpool John Moores), T O'Brien (Manchester), G Schwarz (West Chester), S Starrfield, J-U Ness (Arizona State), J Krautter (Heidelberg), J Drake (SAO), A Evans (Keele), S P S Eyres (Central Lancashire) | Swift observations of the current nova outburst of RS Oph have continued. After the two observations reported in IAUC # 8675 , there have been ~1 ksec observations on the following dates: Feb 21.01, 23.82, 26.43, 28.44, Mar 03.00, 10.82, 13.83.
Between Feb 21.01 and Mar 10.82 the count rate in the 0.3-10 keV band has decreased continuously from 19.8 c/s to 6.0 c/s (Mar 10.82). The X-ray spectrum has shown a diminishing contribution from the hotter components, with a very slight rise at sub-keV energies. The Swift-XRT spectrum has been adequately fit with 3 optically thin components, having temperatures on Feb 21 around 0.2, 0.9 & 6.4 keV, and subsequently decreasing.
The most recent Swift observation (Mar 13.83) showed an increased count rate of 17.6 c/s, the increase being due to a massive rise in flux below 0.6 keV. This new spectral component may be due to strong emission lines from hydrogen-like and helium-like oxygen and nitrogen. Alternatively, this component may be optically thick, and so might represent emission from the hot white dwarf. The XRT spectral resolution at these low energies makes the two possibilities hard to distinguish, a grating observation is needed for this purpose.
When fit with a blackbody absorbed by a strong oxygen edge, a temperature of 1.1e6 K and a radius of 1.6e9 cm resulted. We note that a hot white dwarf atmosphere model fit is required for the determination of reliable physical parameter values however.
Swift observations continue. We thank the Swift MOC team at Penn State University for their efforts. | 2006-03-15 01:03:00 | x-ray,nova | 2006-03-15 | 01:03:00 | 1,568 | [
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] | 763 |
765 | Periodic X-ray modulation in Swift J0732.5-1331 | P. J. Wheatley, T. R. Marsh (Warwick), W. Clarkson (STScI) | We report the results of a Swift timing analysis of the probable new intermediate polar Swift J0732.5-1331 (ATEL #697, #735, #757, #760, and #763). This object was detected as a hard X-ray source with Swift (ATEL #697) and found to have the optical spectrum of a magnetic cataclysmic variable (ATEL #735, #763). A fast optical pulsation was also detected (512.42 s; ATEL #757) leading to its classification as a probable new intermediate polar.
Further analysis of the Swift data reported in ATEL #697 shows that the optical pulsation is detected also in X-rays. The X-ray power spectrum suffers from severe aliasing, but the second highest peak lies precisely at the frequency of the optical pulsation. This strongly supports the classification of Swift J0732.5-1331 as an intermediate polar.
The X-ray modulation is single peaked, in contrast to the optical (ATEL #757). It is strong below 2keV, but absent at higher energies. This is characteristic of photoelectric absorption and is often seen in intermediate polars. Re-analysis of the Swift X-ray spectrum shows that a partial-covering absorption model allows the fitted temperature to drop below that quoted in ATEL #697 to values typical of intermediate polars (kT~20keV).
The Swift ultra-violet power spectra also suffer from severe aliasing, but a strong peak is seen in the UVM2 (2200 Ang) power spectrum precisely at the optical pulsation frequency. No power is seen at the first harmonic, indicating that the ultra-violet modulation is single peaked. | 2006-03-15 02:31:00 | optical,ultra-violet,x-ray,binary,cataclysmic variable,variables | 2006-03-15 | 02:31:00 | 1,516 | [
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] | 764 |
766 | Outburst of IGR J11215-5952 Observed with RXTE | David. M. Smith and Nathan Bezayiff (U. C. Santa Cruz), Ignacio Negueruela (U. Alicante) | Sidoli et al. (2006, astro-ph/0203081) reported that the hard x-ray transient IGR J11215-5952 appeared to have a recurrence period of ~330 days, based on three short outbursts observed by INTEGRAL, the most recent of which was actually the discovery observation (Lubinski et al., ATEL #469). This short outburst, and the presence in the INTEGRAL error circle of the blue supergiant HD 306414 (Negueruela et al. 2005, ATEL #470), suggested that this source is a member of the rapidly growing class of supergiant fast x-ray transients (SFXTs; Negueruela et al. 2005, astro-ph/0511088; Smith et al. 2006, ApJ 638, 974; Negueruela et al. 2006, ApJ 638, 982).
Based on this recurrence period, we suggested monitoring the source with the Rossi X-ray Timing Explorer (RXTE) during the period of March 15 to March 18, 2006, based on the expectation of the next outburst. Five 1-ksec pointings spanning the time from 00:38UT on March 15 to 12:09UT on March 16 show no activity. The next four pointings, ranging from 22:09UT on March 16 to 20:07UT on March 17, show the source to be in outburst. The first observation of activity is 328.7 days after the first activity seen by Lubinski et al., which began on April 22, 2005 at 06:02:25. Counting three periods from the start of first outburst found by Sidoli et al., the period is 329.0 days.
The RXTE/PCA data taken so far show three characteristics typical of SFXT outbursts. First, there is extreme variability: the flux at 13:43UT on March 17 is nearly back to background levels, while the first and last of the four active pointings are the brightest, and nearly equal. Second, the spectrum is hard: the initial pointing is fit well by a power law of photon index (-1.7 +/- 0.2) in the range 2.5-15 keV. In this restricted range, this could be consistent with either a black-hole hard state or an accreting pulsar spectrum. Finally, the best-fit hydrogen absorption column, (11 +/- 3)e22 per cm2, is higher than expected from Galactic absorption; this is also typical of SFXTs.
The peaks of the outburst are at about 2e-10 ergs/cm2/s (absorption removed) from 2-10 keV, corresponding to about 1e36 erg/s at 6.2 kpc (the distance to HD 306414 found by Masetti et al., astro-ph 0512399). This is about 1/3 of the luminosity from 5-100 keV given by Sidoli et al., and so roughly consistent with the other outbursts.
It is not yet known whether the outburst has ended. Another telegram will be posted at that time. In the meantime, prompt observations in the x-ray and at other wavelengths are encouraged. The best-fit position of the x-ray source, given by Sidoli et al., is (RA: 11 21 50.8, Dec: -59 52 48.3). The Tycho position of HD 306414 is (RA: 11 21 46.807, Dec: -59 51 47.93).
This is the first confirmation of a recurrence period in an SFXT candidate. If the proposed link between IGR J11215-5952 and HD 306414 holds up, this period suggests that the difference between SFXTs and persistently bright supergiant x-ray binaries like Cyg X-1 and Vela X-1 may be that the former have long period, elliptical orbits.
We thank RXTE project scientist Jean Swank and the RXTE schedulers for their rapid and positive response to this request. | 2006-03-18 11:57:00 | x-ray,binary,pulsar,transient,request for observations | 2006-03-18 | 11:57:00 | 3,190 | [
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] | 765 |
767 | Orbital Period of Swift J0732.5-1331 | J. R. Thorstensen (Dartmouth), J. Patterson, J. Halpern (Columbia U.), N. Mirabal (U. Michigan) | On the nights of 2006 March 17, 18, and 19 UT we obtained time-series spectroscopy of the optical counterpart of this hard X-ray source (Ajello et al., ATEL #697), using the Hiltner 2.4m telescope at MDM Observatory and the Modular Spectrograph, covering from 4300 to 7500 Angstroms at 3.6 A resolution. The slit was oriented at a position angle of 43 degrees to minimize contamination from the nearby crowding star (Marsh et al., ATEL #760), but the stars were not cleanly resolved. In total, 45 exposures of 8 minutes each were obtained. The observations were arranged to span the greatest possible range in hour angle, on one occasion reaching 4.3 airmasses.
All the spectra show substantial H-alpha emission, which varied substantially in radial velocity, consistent with the findings of Torres et al. (ATEL #763). The variations are periodic; a least-squares sine fit gives 0.2335(8) d and a semiamplitude K = 150(7) km/s, with an rms scatter of 17 km/s. The period choice is unambiguous; the best alternative period at 0.1895 d (corresponding to a different choice of the daily cycle count) gives a significantly worse fit, and a Monte Carlo simulation indicates that it has a negligible likelihood of being the true period. The lack of ambiguity is due to the relatively strong, clean velocity modulation and the wide range of hour angles observed.
The radial velocity modulation almost certainly indicates the orbital period of this object. Other observers have noted a much shorter-period (512.42 s) modulation in the optical (Patterson et al., ATEL #757) and in the X-ray (Wheatley et al., ATEL #765), leading to the classification of this object as an "intermediate polar", or DQ-Her type cataclysmic binary. The orbital period found here is similar to other members of this class and supports this interpretation. | 2006-03-19 21:58:00 | optical,x-ray,binary,cataclysmic variable,star,variables | 2006-03-19 | 21:58:00 | 1,827 | [
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] | 766 |
768 | Swift XRT confirmation of HD 306414 as the counterpart to IGR J11215-5952 | D. Steeghs, M. A.P. Torres (CfA), P. G.Jonker (CfA/SRON) | Following the report of renewed activity in the hard X-ray transient IGR J11215-5952 (ATEL #469, #766), we have obtained a Swift TOO observation of the field covering this X-ray source.
An X-ray Telescope (XRT) observation was obtained during 2006 March 20 18:50-19:02UT in Photon Counting mode with 640s on source. A single faint X-ray source was detected in the field of view with a mean event-rate of 0.05 counts/sec. Its position was determined to be R.A.(J2000): 11:21:46.9, Dec(J2000): -59:51:42 with an estimated error radius of 5 arcseconds. This position is within the 1.2 arcmin INTEGRAL position reported in Sidoli, Paizis & Mereghetti (astro-ph/0603081). The ROSAT archive lists no strong sources within this field of view, and we conclude that the detected XRT source is thus associated with IGR J11215-5952. The XRT position is consistent with the bright supergiant HD306414 and therefore confirms the association proposed by Negueruela, Smith & Chaty (ATEL#470).
For a range of spectral models, we derive an observed 2-10 keV flux close to ~1e-11 ergs/cm2/s. This is significantly below the peak flux reported in ATEL #766 though still well above the expected quiescent luminosity.
We thank the Swift team, in particular Jamie Kennea, for making this observation possible. | 2006-03-21 23:33:00 | x-ray,binary,neutron star,star,transient | 2006-03-21 | 23:33:00 | 1,290 | [
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] | 767 |
769 | Hard X-ray brightening of Ginga 1843+009 seen by Swift/BAT | H. Krimm (GFSC/USRA), L. Barbier (GSFC), S. Barthelmy (GSFC),J. Cummings (GSFC/ORAU), E. Fenimore (LANL), N. Gehrels (GSFC), C. Markwardt (GSFC/UMD), D. Palmer (LANL), A. Parsons (GSFC), T. Sakamoto (GSFC/ORAU), J. Tueller (GSFC) | As part of its hard X-ray transient monitor program, the Burst Alert Telescope on Swift has detected a brightening of the transient X-ray pulsar Ginga 1843+009. The source first became detectable on March 4, 2006, rising to a peak daily average brightness of 0.011 +/- 0.002 counts/s/cm^2, corresponding to ~50 mCrab in the 15-50 keV band, on March 17, 2006. The highest flux seen in a single Swift pointing was 0.044 +/- 0.015 counts/s/cm^2 (220 mCrab) in a 872 s observation starting at 20:24:55 UT on March 14, 2006. The brightness of this source has since declined somewhat to ~30 mCrab on March 21, 2006.
This is the brightest reported outburst of Ginga 1843+009 and the first reported since April 29, 2005 (ATEL #472), when INTEGRAL reported detections at a level of 40 mCrab. An earlier weaker outburst was reported by INTEGRAL in May 2006 (ATEL #159). | 2006-03-22 06:21:00 | x-ray,pulsar,transient | 2006-03-22 | 06:21:00 | 860 | [
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770 | RS Oph: Swift X-ray observations find short period modulation and highly variable low energy flux | J Osborne, K Page, A Beardmore M Goad (Leicester), M Bode (Liverpool John Moores), T O'Brien (Manchester), G Schwarz (West Chester), S Starrfield, J-U Ness (Arizona State), J Krautter (Heidelberg), J Drake (SAO), A Evans (Keele), S P S Eyres (Central Lancashire) | Swift X-ray telescope observations following the recent explosion of the recurrent nova RS Oph over 2006 Mar 17.65 - Mar 19.02 UT have shown a much increased count rate compared to the days before, and have revealed two new forms of modulation.
The Swift XRT 0.3-10 keV light curve can be characterised as a high level of 100-150 c/s which appears to be cut by two deep dips (centred on Mar 18.25 & 18.79 UT) during which the count rate fell below ~20 c/s. These high count rates compare with an initial secular decline to ~6 c/s on Mar 10.82. The increased count rate is due to a higher flux from the new low energy component (E<0.7 keV) reported in ATEL #764. The Swift data do not strongly reject a periodic recurrence of the dips, which are not of uniform width. It is also possible that their apparent separation is due to the ~96 min sampling by Swift; the rest of the light curve is suggestive of aliasing, and a period near 1.7 hours may be present. The high-low flux episodes are visible both above and below 0.7 keV.
The XRT data also show faster modulation at more than one period. Strong modulation (amplitude up to 9%) at periods of 35.0 and 34.5 sec is seen. Other nearby periods may also be present, and the period often changes from one Swift observation to the next. The modulation is quasi-sinusoidal, and has similar fractional depth above and below 0.7 keV. Occasionally a first harmonic is also seen.
The X-ray flux during Mar 20.75 - 22.16 was at a similar level and displayed similar behaviours, including: 3 dips or rapid declines again separated by ~0.54 days; possibly related to this, unresolved variations again suggestive of an underlying ~1.7 hr modulation; and multiple periods around 35 sec.
Throughout the entire interval the harder X-ray flux (E>1.5 keV) shows a declining trend, broadly consistent with the earlier behaviour, and with a slight imprint of the low energy variations in the Mar 22 observation.
The 0.3-10 keV Swift X-ray light curve for the two intervals can be viewed at http://www.star.le.ac.uk/~julo/RSOph/
The substantially increased flux at low energies appears similar to the emergence of the super-soft phase in other novae, caused by the unveiling of the still-burning white dwarf. The origin of the intensity variations at timescales longer than one hour is unclear. The modulation timescales of ~13 hrs and/or 1.7 hrs are both much shorter than those expected for the accretion disk, and RS Oph is thought to be at low inclination (Dobrzycka & Kenyon 1994 AJ 108, 2259).
The poor stability of the ~35 sec periods appears to disfavour an explanation based on the rotation period of the white dwarf. The nova V1494 Aql showed multiple soft X-ray periods, albeit mostly above 1000 sec, attributed by Drake et al 2003 (ApJ 584, 448) to pulsations. Similarly, Ness et al 2003 (ApJ 594, 127) found a soft X-ray period in the nova V4743 Sgr at 1324 sec. Even so, spinning magnetized white dwarfs are known to have short periods (eg AE Aqr at 33 sec), and a number of novae contain rapidly spinning magnetic white dwarfs (eg DQ Her, V533 Her, GK Per).
Swift observations continue, thanks to the efforts of the Swift MOC at Penn State. | 2006-03-23 01:49:00 | x-ray,nova,star,variables | 2006-03-23 | 01:49:00 | 3,193 | [
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771 | Type determination for SN 2006at | A. Gal-Yam (Caltech), A. Cucchiara (Penn State) and P. Capak (Caltech) | A. Gal-Yam, A. Cucchiara and P. Capak report for the CCCP: We have observed SN 2006at (Dintinjana and Mikuz; IAUC # 8687) with the DBSP spectrograph mounted on the Hale 200" telescope at Palomar Observatory on 2006 March 17 UT, under generally poor conditions. Reduction of the spectrum shows Balmer lines superposed on a blue continuum, indicating this is a type II SN, confirming the suggestion of Brown and Immler (Atel #761) based on early Swift photometry. The Halpha profile is strongly dominated by emission, though, an atypical profile for the II-P subtype. The redshift of this event appears to be low (z<0.01) based on the the Balmer lines, but a spectrum of the host galaxy will be required to get an accurate redshift for this event. | 2006-03-24 14:46:00 | optical,supernovae | 2006-03-24 | 14:46:00 | 745 | [
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] | 770 |
772 | Type determination for SN 2006aw | Schuyler D. Van Dyk (Spitzer Science Center/Caltech), Lucy J. Hadfield (Spitzer Science Center/Caltech and Univ. of Sheffield) | S.D. Van Dyk and L.J. Hadfield report: We have observed SN 2006aw (Monard; CBET 434) with the RC Spectrograph on the CTIO Blanco 4-m telescope on 2006 Mar 24.00 UT under very good conditions. Comparing with the spectrum of SN 1990U on day 12 in Matheson et al. (2001, AJ, 121, 1648), from a preliminary reduction of the SN 2006aw spectrum we determine that it is a Type Ic and estimate its age at about two weeks old. From H-alpha in the host galaxy's spectrum, we determine a redshift z=0.019 (cf. z=0.016 listed by NED). | 2006-03-25 01:44:00 | optical,nova,supernovae | 2006-03-25 | 01:44:00 | 522 | [
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] | 771 |
773 | End of outburst of IGR J11215-5952; possible pulsations | David M. Smith, Nathan Bezayiff (U. C. Santa Cruz), and Ignacio Negueruela (U. Alicante) | The recent outburst of IGR J11215-5952, predicted by the ephemeris of Sidoli et al. (2006, astro-ph/0603081) and observed with the Rossi X-ray Timing Explorer (RXTE) (Smith, Bezayiff and Negueruela 2006, ATEL #766) has apparently ended. The first and last observations that showed significant activity began and ended on 22:09UT March 16 and 21:48UT March 18, respectively. Each observation lasted about 1000 s, and three per day were taken from March 15 through March 18. Four later pointings were taken at longer intervals to make certain the outburst had ended. The lower and upper limits to the total duration of the outburst are 2.0 and 3.4 dy. This is similar to the 2004 observation reported by Sidoli et al. 2006. The lightcurve of the outburst is shown in Figure 1 at the link below, including the time at which the Swift X-ray telescope observed the field and found that the companion is indeed the supergiant HD 306414 (Steeghs, Torres and Jonker 2006, ATEL #768) as suggested by Negueruela, Smith and Chaty (ATEL #470).
Several of the pointings show variability which suggests a pulsation period of approximately 195 +/- 10 s. It is clearest in the brightest pointing; that lightcurve, with 1-second binning, is shown in Figure 2 at the link below. We have not been able to connect the observations coherently in phase. An x-ray pulsar with an orbital period of 329 dy and a spin period of 195 s would lie neatly among the Be/NS binary systems on the Corbet diagram correlating spin and orbital periods (Corbet 1986, MNRAS 220, 1047) and far from the supergiant systems. The Swift result clearly associates this transient with a supergiant, however, and the fast, highly variable outburst is consistent with other supergiant fast x-ray transients (SFXTs), not Be/NS systems.
The spectra were hard and changed little through the outburst. A power law, a power law with exponential cutoff (Sidoli et al. 2006), and a thermal bremsstrahlung spectrum all give acceptable fits. The absorption column seemed to drop after the first pointing in outburst, from (11 +/- 3)e22 per cm2 to a level about 1/3 to 1/2 of that during subsequent outburst intervals. Note, however, that the absorption is difficult to measure due to the need to subtract the soft Galactic diffuse emission from the spectrum. The spectrum from the third pre-outburst pointing, which had the lowest flux, was used as background.
We thank Jean Swank and Rudy Wijnands for discussions about the apparent pulsation in the source.
Erratum: The paper of Sidoli et al. 2006, which has been accepted by Astronomy and Astrophysics Letters, was given an incorrect citation in ATEL #766. Its correct listing on the arXiv.org preprint server is astro-ph/0603081, not astro-ph/0203081. | 2006-03-25 03:58:00 | x-ray,binary,pulsar,transient,variables | 2006-03-25 | 03:58:00 | 2,752 | [
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] | 772 |
774 | SGR 1900+14: Swift-BAT detection of renewed activity of a Soft Gamma Repeater | D. M. Palmer (LANL), C. B. Markwardt (GSFC/UMD), and S. D. Barthelmy (GSFC) | As reported in GCN #4922 (Vetere et al.): At 20:16:40 on 25 Mar 2006 UT, the Swift Burst Alert Telescope (BAT) triggered and located a burst from SGR 1900+14 (trigger=202746). The BAT on-board calculated location is RA,Dec 286.828, +9.270 {19h 07m 19s, +09d 16' 11"} (J2000) with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). This position is consistent with SGR 1900+14 (3.3 arcminutes). The BAT light curve shows a single spike with a FWHM less than 128 msec at T_zero. The peak count rate was ~1600 counts/sec (15-350 keV), at ~0 sec after the trigger. This Soft Gamma-ray Repeater has not been active since late 2002. This source is being followed up by Swift as a Target of Opportunity. | 2006-03-26 05:14:00 | gamma ray,soft gamma-ray repeater | 2006-03-26 | 05:14:00 | 733 | [
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] | 773 |
775 | Identification of the X-ray transient Swift J061223.0+701243.9 | D. Grupe (PSU), J. P. Osborne (U Leicester), K. L. Page (U Leicester), D. N. Burrows (PSU), J. A. Nousek (PSU), and D. P. Schneider (PSU) | We report on the optical identification of the X-ray transient Swift J061223.0+701243.9 (Grupe et al., 2006, GCN #4672, GCN #4681) which is an uncatalogued object discovered serendipitously by the Swift X-ray Telescope (XRT) while observing the Swift Burst Alert Telescope (BAT) trigger 180274 (Grupe et al. 2006, GCN #4663) on 2006 February 04 starting 20:35 UT. Note that this X-ray transient was not the cause of the trigger. The X-ray position is 8 arcmin away from the BAT position, outside the BAT 3.6 arcmin error circle (Sakamoto et al. 2006, GCN #4679). Swift-XRT observed Swift J0612+7012 again for ~8 ks on 2006 March 06, starting at 09:21 UT over a period of about 13 hours. The spectrum during this time was well modelled by an absorbed power-law, with Gamma = 1.61 ± 0.24 and NH = (1.8 ± 0.8) x 10^{21} cm^-2 (90% containment). The mean count-rate was approximately 0.053 counts s^-1, corresponding to an observed (unabsorbed) flux of 3.20 (3.92) x 10^-12 ergs cm^-2 s^-1 in the 0.3-10 keV band. During this observation the source count rate increased from 0.05 to 0.08 counts/s over 9.6 hours, then fell over 3.2 hours to 0.03 counts/s. The results of the spectral and temporal analysis are in good agreement with those of the discovery observation of 2006 February 04. Swift J061223.0+701243.9 was observed on 2006 March 21 starting at 02:27 UT with the Low-Resolution Spectrograph (LRS) at the Hobby-Eberly-Telescope (HET) at McDonald Observatory for 3 times 15 minutes using grism #1 with a 2" slit. The spectral resolution was 17A. The optical spectrum clearly shows strong hydrogen and helium emission lines, identifying this source as an X-ray binary system, either a low-mass X-ray binary or a Cataclysmic Variable. H-beta and H-alpha are clearly resolved and we found FWHM=900 km/s, while H-gamma and He II (4686) are clearly detected but the line widths are not resolved. We also found He I at 4471A and 5876A. The line widths, however, are not well-determined. Apart from the emission lines, the continuum is essentially featureless. The optical position measured from the Swift UV-Optical telescope (UVOT) coadded U image is: RA-2000: 06 12 22.6 ± 0.5" Dec-2000: +70 12 43.4 ± 0.8" The UVOT determined the following observed magnitudes on 2006 March 06: V = 19.36+/-0.21 B = 19.69+/-0.15 U = 18.67+/-0.07 UVW1 = 19.05+/-0.08 UVM2 = 19.61+/-0.08 | 2006-03-28 00:13:00 | optical,ultra-violet,x-ray,binary,cataclysmic variable,transient,variables | 2006-03-28 | 00:13:00 | 2,374 | [
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] | 774 |
776 | SWIFT observation of SN 2006bc | S. Immler, Goddard Space Flight Center, NASA, and Universities Space Research Association, and P. J. Brown, Pennsylvania State University, on behalf of the Swift-satellite team | We report on Swift Ultraviolet/Optical Telescope (UVOT) observations of SN 2006bc (Martin CBET #446) obtained on 2006-03-27.93 UT.
A new object is detected at R.A. = 7h21m16s.50, Decl. = -68o59'57".3 (equinox 2000.0) when compared to DSS images, consistent with the position reported by Martin (CBET #446). UVOT magnitudes are B = 17.6, U = 16.7, UVW1 [181-321 nm] = 17.4, and and UVW2 [112-264 nm] = 18.0. Statistical and systematical errors are 0.1 mag each. Comparing the U-B color with other SNe from Poznanski et al. (2002, PASP, 114, 833) shows that the SN is approx. one magnitude bluer than observed in the displayed SNe. The similarity of the colors with the type II-P SN 2005cs (Brown et al. in prep.) and the Type II SN 2006at (Brown & Immler ATel #771) at similar epochs indicate that SN 2006bc is a Type II SN.
Further Swift observations are scheduled. | 2006-03-28 14:49:00 | optical,ultra-violet,supernovae | 2006-03-28 | 14:49:00 | 867 | [
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] | 775 |
777 | Chandra Localization of the Neutron Star X-Ray Transients XTE J1739-285 and XTE J1701-462 | Miriam I. Krauss (MIT), Adrienne M. Juett (U. Virginia), Deepto Chakrabarty (MIT), Peter G. Jonker (CfA/SRON), and Craig B. Markwardt (GSFC/U. Maryland) | We observed the neutron star soft X-ray transients XTE J1701-362 and XTE J1739-285 on 2006 March 27 with the Chandra X-Ray Observatory's High-Resolution Camera (HRC-S) in timing mode, as part of an existing program for the precise localization of neutron star/soft X-ray transients.
The transient Z source XTE J1701-462 has been active since its discovery in 2006 January (ATels #696, #725, #748). We observed the source with Chandra on March 27 for 1140 s beginning at 03:40 UT. The mean count rate was 64.1(2) ct/s. For the spectral shape previously measured by Swift/XRT (ATel #704), this corresponds a flux of 7.6e-9 erg/cm^2/s (0.5-10 keV). The best-fit source coordinates are: R.A. 17:00:58.46, Decl. -46:11:08.6, equinox J2000.0, with an error radius of 0.6 arcsec (90-percent confidence). This position is coincident with the proposed optical (ATel #706), infrared (ATel #712), and radio (ATel #710) counterparts for this source. However, it is inconsistent with the 5.8-arcsec Swift/XRT position error circle (ATel #702), lying 15.4 arcsec from its center.
The transient X-ray burster XTE J1739-285 (IAUC # 7300 ; ATel #622) was discovered in 1999, and the most recent new outburst was reported in 2005 August (ATel #592). We observed the source with Chandra on March 27 for 1156 s beginning at 03:04 UT. The mean count rate was 2.65(5) ct/s. Assuming an absorbed power-law spectrum with photon index 2 and a Galactic absorption column density of 7.8e21 cm^-2, this corresponds to a flux of 1.2e-10 erg/cm^2/s (0.5-10 keV). The best-fit source coordinates are: R.A. 17:39:53.95, Decl. -28:29:46.8, equinox J2000.0, with an error radius of 0.6 arcsec (90-percent confidence). This is consistent with the 6-arcsec Swift/XRT position error circle (ATel #602). | 2006-03-29 05:39:00 | radio,optical,x-ray,binary,neutron star,star,transient | 2006-03-29 | 05:39:00 | 1,767 | [
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] | 776 |
778 | Detection of Type I X-ray burst from IGR J17254-3257 | S. Brandt, C. Budtz-Jørgensen, J. Chenevez (Danish National Space Center) | A type I X-ray burst from IGR J17254-3257 (1RXS J172525.5-325717) has been found in archival data from INTEGRAL. The burst occurred on Feb 17, 2004 at 19:44:00 (UTC) and was detected by the JEM-X X-ray monitor. The burst had a rise time <5s and an e-folding decay time of 15 sec. The burst reached a peak flux of 0.8 Crab in the JEM-X energy band 3-30 keV. The derived position RA=17h25m27s DEC=-32d57'50', with an error radius of 1' is consistent with the position of the ROSAT source 1RXS J172525.5-325717, which is identified as a candidate counterpart for IGR J17254-3257 (ref. J.B. Stephen et al., A&A 432, L49, 2005). | 2006-03-29 17:54:00 | x-ray,neutron star,star | 2006-03-29 | 17:54:00 | 623 | [
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] | 777 |
779 | Swift/BAT and RXTE/ASM Discovery of the Orbital Period of IGR J16418-4532 | R. Corbet (GSFC/USRA), L. Barbier (GSFC), S. Barthelmy (GSFC), J. Cummings (GSFC/NRC), E. Fenimore (LANL), N. Gehrels (GSFC), D. Hullinger (UMD), H. Krimm (GSFC/USRA), C. Markwardt (GSFC/UMD), D. Palmer (LANL), A. Parsons (GSFC), T. Sakamoto (GSFC/NRC), G. Sato (ISAS), J. Tueller (GSFC), on behalf of the Swift-Survey team, and R. Remillard (MIT) | The Swift Burst Alert Telescope (BAT) light curve of IGR J16418-4532 (Tomsick et al. 2004 ATEL #224) obtained between 2004 Dec 21 and 2005 Sep 17 shows modulation at a period near 3.75 days. This period is confirmed and refined by observations made with the Rossi X-ray Timing Explorer All-Sky Monitor (ASM) between 1996 Jan 9 and 2006 March 16.
The mean BAT count rate of IGR J16418-4532 in the range 14 - 195 keV is 9.5 (+/- 0.9 statistical) E-4 counts/s/cm^2 which corresponds to approximately 3 mCrab. The mean count rate in the ASM in the range 1.5 - 12 keV is 0.39 +/- 0.01 (statistical) counts/s, equivalent to approximately 5 mCrab. However, IGR J16418-4532 is located only 0.7 degrees from the ~380 mCrab source GX 340+0. For the ASM this may lead to some contamination of the measured flux from IGR J16418-4532 by emission from GX 340+0.
The parameters of the modulation were quantified by fitting sine waves to the BAT and ASM light curves separately. For the BAT light curve the fit gives amplitude = 9.2 (+/- 1.2 ) E-4 counts/s/cm^2, period = 3.753 +/- 0.004 days, and epoch of maximum flux = MJD 53560.7 +/- 0.1. A sine wave fit to the ASM light curve gives amplitude = 0.09 +/- 0.02 counts/s, period = 3.7389 +/- 0.0004 days and epoch of maximum flux = MJD 53560.2 +/- 0.2. Although the period and epoch derived from the two data sets are formally statistically discrepant, the error bars may well be underestimates because of the presence of non-periodic modulation in the light curves and because the modulation is unlikely to be exactly sinusoidal. The BAT light curve when folded using the parameters derived from the ASM does indeed show modulation similar to that seen when the light curve is folded on the BAT-derived parameters.
We interpret this modulation as revealing the orbital period of a binary system. We note that the mean BAT flux at phase 0.5 is consistent with zero which may indicate the presence of a total eclipse. If there is a total eclipse, then the ~0.25 counts/s detected with the ASM at this phase implies that the background subtracted luminosity in the ASM energy band is about 1.5 mCrab. IGR J16418-4532 lies close to the Galactic plane and a number of sources found with INTEGRAL have been found to be high-mass X-ray binaries with supergiant primaries. The possible presence of an eclipse in the folded light curve is consistent with a supergiant classification. | 2006-03-30 01:44:00 | x-ray,gamma ray,binary,neutron star,pulsar,star | 2006-03-30 | 01:44:00 | 2,414 | [
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780 | XTE J1709-462: Swift/XRT refined position | J. A. Kennea (PSU), O. Godet (U Leicester) and D. N. Burrows (PSU) on behalf of the Swift/XRT team: | In response to the work of Krauss et al. (ATEL #777), we have performed a refined analysis of the Swift/XRT data on XTE J1701-462. We find a refined XRT position for XTE J1709-462 of R.A. = 17:00:58.3, dec. = -46:11:09.0, with a 6.1 arcsecond error radius (90% containment). This refined position lies 1.7 arcseconds from the Chandra position reported in ATEL #777. We therefore conclude that the Swift/XRT position of XTE J1709-462 is consistent with the Chandra reported position. | 2006-03-30 04:44:00 | x-ray,transient | 2006-03-30 | 04:44:00 | 482 | [
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781 | Correction: XTE J1701-462: Swift/XRT refined position | J. A. Kennea (PSU), O. Godet (U Leicester) and D. N. Burrows (PSU) on behalf of the Swift/XRT team: | Correction: Incorrect source name was given in ATEL #780, we apologize for this error. In response to the work of Krauss et al. (ATEL #777), we have performed a refined analysis of the Swift/XRT data on XTE J1701-462. We find a refined XRT position for XTE J1701-462 of R.A. = 17:00:58.3, dec. = -46:11:09.0, with a 6.1 arcsecond error radius (90% containment). This refined position lies 1.7 arcseconds from the Chandra position reported in ATEL #777. We therefore conclude that the Swift/XRT position of XTE J1701-462 is consistent with the Chandra reported position. | 2006-03-30 04:51:00 | x-ray,transient | 2006-03-30 | 04:51:00 | 569 | [
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782 | RTT150 high resolution spectral observations of Solar Corona during the solar eclipse on March 29, 2006 | I. F.Bikmaev, N. A.Sakhibullin, A. I.Galeev (Kazan State University and Academy of Sciences of Tatarstan, Russia), I. M.Khamitov, Z. Aslan (TUBITAK National Observatory, Turkey), R. A.Sunyaev (MPA, Garching, IKI, Moscow) | On March 29, 2006, the total solar eclipse had a duration of totality of about 2 minutes at TUBITAK National Observatory, Antalya, Turkey. The Russian-Turkish 1.5-meter optical telescope (RTT150) equipped with a coude-echelle spectrometer and a 1040 x 1160 pixels nitrogen cooled CCD was used to get the spectra of solar Corona. We have obtained two high-resolution, high S/N spectra of a small region of the solar Corona situated approximately 3 arcmin Eastwards of the solar limb, with coordinates R.A.(2000.0) = 00h 32m 37s, Dec.(2000.0) = +03o 23' 55". Target uncertainty is about 10-20 arcsec. The size of the entrance slit was 3 x 1.5 arcsec, the spectral resolution R ~ 40000 and the spectral range ~ 3900 - 8600 A, with some gaps in the visual and near infrared regions. The exposure time was 30 sec each and middle time of exposures are UT = 10:54:33 and UT = 10:55:44 ( http://www.tug.tubitak.gov.tr/~irekk/eclipse2006/ut105433.jpg , http://www.tug.tubitak.gov.tr/~irekk/eclipse2006/ut105544.jpg ). Preliminary spectra processing reveals the presence of several known Coronal and Chromospheric emission lines ( strong Fe X 6374, Fe XIV 5303, Fe XI 7892, Ar X 5534, weak Ca XV 5694, He I, H I, strong K and H Ca II, weak Ca II 8542, etc). In both spectra there are many weak absorption lines as well as several weak emission lines. The FWHM of the strong emission lines is 30-40 km/sec (at 7-10 km/sec of spectral resolution). Note that the intensity of Coronal emission lines is almost identical in both spectra, in contrast with considerable decrease in chromospheric lines intensity in the second spectrum. ( http://www.tug.tubitak.gov.tr/~irekk/eclipse2006/fe7892.jpg , http://www.tug.tubitak.gov.tr/~irekk/eclipse2006/halpha.jpg ) Our targeting point was far away ( ~ 0.2 Solar Radius) from the limb, i.e. very far from the chromosphere. We suppose that, probably, by chance we have observed the spectrum of an errupting prominence detail situated within the line-of-sight during our observations. | 2006-03-30 20:38:00 | optical,the sun | 2006-03-30 | 20:38:00 | 2,011 | [
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] | 781 |
783 | Optical classification of 8 INTEGRAL sources | N. Masetti (INAF/IASF, Bologna), L. Morelli (PUC, Santiago), E. Palazzi, J. Stephen (INAF/IASF, Bologna), A. Bazzano (INAF/IASF, Rome), A. J. Dean (Univ. Southampton), R. Walter (ISDC, Versoix) and D. Minniti (PUC, Santiago) | On 20-22 March 2006 we used the R-C spectrograph of the CTIO 1.5m telescope in Cerro Tololo (Chile) to get optical spectra of the putative counterparts of 8 X-ray sources discovered by INTEGRAL (see Bird et al. 2006, ApJ, 636, 765; Halpern 2005, ATel #572; Kuiper et al. 2006, ATel #684; Sazonov et al. 2005, A&A, 444, L37; Revnivtsev et al. 2006, Astron. Lett., 32, 145).
To reduce the X-ray error box size to a few arcsec at most, we selected sources with a single ROSAT Bright Source (Voges et al. 1999, A&A, 349, 389), and/or a single Swift/XRT archival X-ray source (available at http://www.asdc.asi.it ), or a single Chandra source within the INTEGRAL error box (which, according to Stephen et al. 2006, A&A, 445, 869, means that this is very likely the soft X-ray counterpart of the INTEGRAL source). In one case (AX J1700.2-4220) we chose a known emission-line star in the INTEGRAL error box as the putative counterpart; for the caveats regarding this choice, we refer the reader to Masetti et al. (2006, A&A, in press [astro-ph/0512399]). Exposure times ranged from 40 to 60 minutes, depending on the object brightness.
Notes on individual sources (coordinates refer to epoch J2000):
IGR J05007-7047: the presence of Halpha emission and the rest of the Balmer lines in absorption, at a redshift consistent with that of the LMC, suggests that this is likely a HMXB located in this galaxy.
XSS J12270-4859: the only object in the error boxes of 1RXS J122758.8-485343 and of the XRT observation, USNO-A2.0 source U0375_15949017 (RA = 12 27 58.77, Dec = -48 53 42.8), shows Balmer and HeI lines in emission at z = 0. Given the similarity with the optical spectrum of IGR J00234+6141 (Bikmaev et al. 2006, Astron. Lett., in press [astro-ph/0603715]) we classify it as a CV.
IGR J14536-5522: the brightest object in the XRT and ROSAT error boxes (Mukai et al. 2006, ATel #686), USNO-A2.0 source U0300_22436308 (RA = 14 53 41.16, Dec = -55 21 37.4), shows a spectrum which is similar to that of XSS J12270-4859. Thus we classify it as a CV.
IGR J15094-6649: as for the two previous cases, we classify the USNO source U0225_21896607 (RA = 15 09 26.00, Dec = -66 49 23.4), contained within the 1RXS J150925.7-664913 source error box, as a CV due to the emissions in its optical spectrum.
IGR J16167-4957: Balmer, HeI and HeII emissions at z = 0 observed in the only optical source within the XRT error circle, USNO-A2.0 object U0375_26829054 (RA = 16 16 37.78, Dec = -49 58 44.7), suggest that the spectrum is typical of a CV.
IGR J16207-5129: in the XRT error box, the USNO-A2.0 object U0375_27093111 (RA = 16 20 46.28, Dec = -51 30 06.3) shows an Halpha emission at redshift 0 superimposed on a reddened continuum. The optical spectrum is similar to that of 2RXP J130159.6-635806 (see Masetti et al. 2006, A&A, in press [astro-ph/0512399]); thus, the source is likely a HMXB. We also correct the identification of IGR J16207-5129 reported in the above paper, where this object was associated with star HD146803.
AX J1700.2-4220: our spectrum of star HD153295 within the INTEGRAL error box confirms its emission-line nature (e.g. Merrill & Burwell 1943, ApJ, 98, 153). The optical spectrum of this star points to a HMXB nature. However, as no arcsec-sized X-ray position is available, we consider the association as tentative.
IGR J17195-4100: the only object consistent with the error boxes of source 1RXS J171935.6-410054 and of the XRT pointing, USNO-A2.0 object U0450_27095307 (RA = 17 19 35.91, Dec = -41 00 53.7), shows Balmer and He emissions at z = 0, similarly to the CVs described above.
We thank C. Aguilera and A. Gomez for assistance at the telescope. | 2006-03-31 05:06:00 | optical,x-ray,binary,cataclysmic variable,star,variables | 2006-03-31 | 05:06:00 | 3,676 | [
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] | 782 |
784 | Optical and NIR observations of XTE J1739-285 | M. A. P. Torres, D. Steeghs, M. R. Garcia, J. E. McClintock (CfA), P. G. Jonker (SRON/CfA), D. Kaplan (MIT), J. Casares (IAC), R. Greimel (ING), T. Augusteijn (NOT) | We report optical and near-infrared (NIR) observations of the field containing the neutron star X-ray transient XTE J1739-285 (IAUC # 7300 , ATel #622). The recently reported Chandra localization (ATel #777) provides a significant improvement over the Swift XRT position reported in ATel #602, facilitating the identification of potential counterparts.
Optical observations were performed on 2005 Aug 30 20:59-21:14 UT and 2005-09-16 20:39-20:55 at the 2.56-m Nordic Optical Telescope (NOT) on La Palma using ALFOSC. On Aug 30 we acquired three 180s R-band images under seeing conditions of 0.8 arcsec (note that these observations were reported in ATel #602 with a wrong observing date). On Sep 16 several R-band images ranging in exposure times between 130 and 200s were obtained with a seeing of 0.8 arcsec. The images were flux calibrated using Landolt standards.
The NIR observations consist of a series of Ks-band images obtained with the 6.5m Magellan Baade telescope on 2005 Sep 13 00:10-01:01 and 2005 Oct 20 23:44-23:56 using the PANIC camera and totaling 900s and 225s on source respectively. The frames were acquired with a variable seeing ranging from 0.5-0.8 arcsec during the night of Sep 13 and 0.4 arcsec during Oct 20. Photometric and astrometric scales were defined using 2MASS sources in the field of view.
No optical counterpart is found in the NOT images down to a 3-sigma detection limit of R > 21.5 (Aug 30) and R > 22.5 (Sep 16). We remark here that the Aug 30 images were obtained at the peak of X-ray activity in 2005 (ATel #592) whereas the Sep 16 images were acquired after this event. Taking into account the 0.5 Crab flux reported during type I X-ray bursts (ATel #622) which must be below or equal to the Eddington Luminosity, we derive a (rough) upper limit on the distance to XTE J1739-285 of 12 kpc. This translates into an upper limit R-band absolute magnitude of M_R > 3.2 during the peak of X-ray activity and this suggests an intrinsically faint transient. Here we have used A_R=2.9 mag as expected from the hydrogen column towards the source (NH=7.4e21 cm**-2: Dickey & Lockman 1990).
Two NIR sources are visible inside the Chandra error circle for XTE J1739-285. The sources have approximate magnitudes of Ks = 16.9 +/- 0.2 and 17.8 +/- 0.3. We could not establish significant variability in either of these two sources. Using the above constraint on the distance and reddening (A_K=0.4), we derive M_K > 1.1 and 2.0 for the absolute magnitude in the K-band. However, the positional coincidence of both sources is insufficient to establish any of them as the counterpart to XTE J1739-285; a K5V (M2V) field star at 2 kpc would have an apparent magnitude of 16.9 (17.8) and 21.2 (22.9) at the K- and R-bands respectively.
Further NIR photometry to search for variability during quiescence and/or outburst is required to confirm/reject any of the above candidates. | 2006-03-31 05:13:00 | infra-red,optical,x-ray,binary,neutron star,star,transient,variables | 2006-03-31 | 05:13:00 | 2,908 | [
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] | 783 |
785 | Optical classification of 3 Swift southern hard X-ray sources | L. Morelli (PUC, Santiago), N. Masetti, L. Bassani, R. Landi, A. Malizia (INAF-IASF, Bologna), A. J. Bird (Univ. Southampton), P. Ubertini (INAF-IASF, Rome) and G. Galaz (PUC, Santiago) | In order to identify the nature of 3 hard X-ray sources recently discovered by Swift (see ATels #669 and #677), we acquired optical spectra of their counterparts at the 1.5m telescope of the Cerro Tololo Interamerican Observatory (Chile) using the R-C spectrograph on the nights of March 21 and 22, 2006. Total exposure times ranged from 15 to 40 minutes, depending on the object brightness.
In the following table, we report the classification of these sources:
Notes on individual sources.
SWIFT J0601.9-8636: from the proposed optical counterpart, the nucleus of galaxy LEDA 18394, we detect narrow emission lines of Halpha and [OIII] superimposed on a continuum resembling that typical of spiral galaxy. This possibly indicates that the nucleus might be a hidden Sy2 AGN. We however caution the reader about the certainty of the association between the high-energy source detected with Swift/BAT and the galaxy (Tueller et al., ATel #677). The measured redshift is z = 0.006 +- 0.001, consistent with that measured by Fisher et al. (1995, ApJS, 100, 69).
SWIFT J1038.8-4942: broad Halpha and Hbeta emissions plus narrow [OI] and [OIII] emission lines are detected on a relatively flat continuum in the optical spectrum of the counterpart, 2MASX J10384520-4946531 (Tueller et al., ATel #669). From the observed wavelengths of narrow features, we determine a redshift z = 0.060 +- 0.001. The overall spectral appearance allows us to classify this object as a Seyfert 1 galaxy.
SWIFT J1238.9-2720: the presence of Halpha, Hbeta, [NII] and [OIII] narrow emission lines are detected in the optical spectrum of the counterpart, galaxy ESO 506-G027. The overall spectrum indicates that this source is most likely a Seyfert 2 AGN. The features are at redshift z = 0.024+-0.001, consistently with Da Costa et al. (1998, AJ, 116, 1).
We thank C. Aguilera and A. Gomez for the assistance at the telescope | 2006-03-31 05:14:00 | optical,x-ray,agn | 2006-03-31 | 05:14:00 | 1,903 | [
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] | 784 |
786 | Orbital Parameters for the X-Ray Pulsar IGR J16393-4643 | Tommy Thompson, John A. Tomsick, Richard Rothschild (CASS/UCSD), Jean in 't Zand (SRON), and Roland Walter (ISDC) | With recent and archival Rossi X-ray Timing Explorer (RXTE) X-ray measurements of the heavily obscured X-ray pulsar IGR J16393-4643, we carried out a pulse timing analysis to determine the orbital parameters. Assuming circular orbits, we phase-connected data spanning over 1.5 years. The most likely orbital solution has a projected semi-major axis of 43 +/- 2 lt-s and an orbital period of 3.688 +/- 0.001 days. This implies a mass function of 6.5 +/- 1.1 solar masses and confirms that this INTEGRAL source is a High-Mass X-ray Binary system. By including eccentricity in the orbital model, we find e < 0.25 at the 2-sigma level. The 3.7 day orbital period and the previously known ~910 s pulse period place the system in the region of the Corbet diagram populated by supergiant wind accretors, and the low eccentricity is also consistent with this type of system. Finally, it should be noted that although the 3.7 day orbital solution is the most likely one, we cannot completely rule out two other solutions with orbital periods of 50.2 and 8.1 days. | 2006-04-01 01:35:00 | x-ray,binary,neutron star,pulsar,star | 2006-04-01 | 01:35:00 | 1,054 | [
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] | 785 |
787 | Optical Outbursts from SDSS J113551.09+532246.2 and SDSS J120231+450349 | R. Quimby and P. Mondol (U. Texas) | We report the discoveries of two optical transients found in unfiltered CCD images taken by the 0.45m ROTSE-IIIb telescope at the McDonald Observatory. The first object was detected on 2006 March 24.40 UT (about 15.1 mag) at RA = 11h35m51.12s, DEC = +53o22'46.1" (J2000; uncertainty +/- 0.5"). This position matches the source SDSS J113551.09+532246.2, observed in quiescence by Sloan at r= 20.71. This object was not detected by ROTSE-IIIb on Mar. 22.14 (limiting mag about 16.9), nor on a co-addition of images taken between 2005 Apr. 12 and 2006 Feb 4 (limiting mag about 18.4). The object was about 15.2 mag on Mar 25.13, and then faded to about 15.8 mag on Mar. 26.1. The object was not detected in ROTSE-IIIb images taken on Mar. 30.12 (limiting mag 16.7) nor on Mar. 31.23 (limiting mag 17.8). The object was also caught during outburst in the USNO B1.0 catalog (R2 = 15.05 mag). We tentatively classify SDSS J113551.09+532246.2 as a dwarf nova.
The second object was detected Mar. 21.15 (about 13.4 mag), and is located at RA = 12h02m30.99s, DEC = +45o03'48.7" (J2000; uncertainty +/- 0.5"). This source matches the known cataclysmic variable SDSS J120231+450349 (Szkody, P. et al. 2006, AJ, 131, 973), which is listed at r=19.92 mag. The object was not detected in ROTSE-IIIb images taken on Mar. 7.19 (limiting mag 17.5), and it has faded over the last 10 days (Mar. 25.15, 13.9 mag; Mar. 31.28, 14.8 mag).
Finding Chart for SDSS J113551.09+532246.2
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] | 786 |
788 | Swift XRT detection of the Integral ISGRI source IGR J2018+4043. | J. Kennea, G. G. Pavlov (PSU), A. M. Bykov, A. M. Krassilchtchikov, Yu. A. Uvarov (Ioffe Inst.), F. Lebrun (CEA-Saclay), H. Bloemen, W. Hermsen, J. Kaastra (SRON) | We observed the field around the hard X-ray source IGR J2018+4043 (Bykov et al. 2004, A&A, 427, L21) with Swift (total exposure 5 ks) and detected a point-like source in the XRT image at R.A. = 20:18:38.5, decl. = +40:41:00.4 (uncertainty 4.2 arcsec radius at 90% confidence level), consistent with the ISGRI position and possibly with the position of the unidentified CGRO EGRET source 3EG J2020+4017. The observed 0.5-10 keV flux is 3(+/-1)e-12 erg/cm^2/s. A power-law fit of the spectrum gives a photon index Gamma = 0.7(+2.2,-0.2) and hydrogen column density NH = 4(+6/-3)e22 cm^{-2} (90% confidence errors). We found a likely NIR counterpart of the source in the 2MASS catalog centered at R.A. = 20:18:38.73, decl. = +40:41:00.1 (2.6 arcsec from the XRT position), with magnitudes J=14.9, H=12.7, Ks=12.1 (as the 2MASS source shows some evidence of extension, the quoted magnitudes may need to be corrected). The source could be an AGN or a Galactic X-ray binary. Deeper X-ray observations are needed to distinguish between these interpretations. | 2006-04-04 04:41:00 | infra-red,x-ray,gamma ray,agn,binary | 2006-04-04 | 04:41:00 | 1,051 | [
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] | 787 |
789 | Swift-BAT observations of SGR 1900+14 | D. M. Palmer (LANL), T. Sakamoto (GSFC/ORAU), S. Barthelmy (GSFC), J. Cummings (GSFC/ORAU), N. Gehrels (GSFC), H. Krimm (GSFC/USRA),C. Markwardt (GSFC/UMD), J. Tueller (GSFC) | The recent re-activation of the Soft Gamma-ray Repeater SGR 1900+14 (Vetere et al. GCN# 4922) has been intensively observed by the Swift Burst Alert Telescope (BAT) as well as by the Swift UVOT and XRT instruments. Here we report on the BAT results.
The first detection by BAT was at 2006-03-25 10:12:04 UTC, and marked the first detection of a burst from this source since 2003 (C. Kouveliotou, priv. comm.) The most recent burst was 2006-03-29 12:19:51 (as of 2006-04-03 11:00). A total of 22 bursts or burst sequences have been identified by the onboard software (where a burst sequence is defined as a set of bursts separated from other detected bursts by at least 5 minutes, including gaps due to observational and instrumental effects).
In the 5 months before this latest round of activity, the upper limit to steady-state emission on individual days with good observations of this source is 30 mCrab (3 sigma). In the 9-month interval 2004-12-15 to 2005-09-15, the long-term average steady-state emission is less than 1.4 mCrab (5 sigma).
The greatest intensity of activity was during an interval starting before 2006-03-29 02:38:10 (when the SGR entered the BAT field of view) to 02:59:43 (beyond which there is no detected activity through the end of the pointing at 03:13:11). Within this time period there is a considerably more intense interval, 2:53:10 - 2:53:42, which we will call the storm. Event-by-event data is available for most of this storm period.
The storm contains both wide and narrow peaks. The narrow peaks have typical widths of 10-100 ms and peak rates up to 400 counts/ms. The wide peaks have peak rates falling in the narrow range of 400-850 counts/ms and durations of up to 1.5 seconds. (All rates are ~12-100 keV measured on 1 ms timescales with approximately 2300 cm^2 effective area).
The wide peaks typically show a rapid rise (<10 ms) to near the maximum value, a somewhat steady decline (at rates of ~1 count/ms/ms), sometimes with instances of re-energization, to an inflection point typically at a rate around 200-400 counts/ms, followed by a precipitous drop over the next ~10 ms.
For spectroscopy, data from the narrow peaks were accumulated into a single spectrum for analysis, while the wide peaks were analyzed with time-resolved spectra.
The accumulated spectrum of short peaks is well fitted with an optically thin thermal bremsstrahlung spectrum (OTTB), a power-law times an exponential cutoff model (CPL), and a sum of two blackbodies model (2BB). A single blackbody model shows a bad fit. kT of OTTB is 21 keV. In 2BB model, the temperatures are 4.6 keV and 11.2 keV.
The time-resolved spectra of the bright peaks are well fitted in CPL and 2BB. But they show a bad fit in OTTB model, especially at the bright part. However, if we ignore below spectral bins 30 keV, OTTB model shows an acceptable fit with temperatures consistent with the Konus-Wind, RXTE and BATSE observations (Aptekar et al, ApJS, 137, 227; Ibrahim et al. ApJ, 558, 237). The temperatures and the blackbody radii in 2BB model are consistent with the HETE-2 parameters (2001 activity; Olive et al., ApJ, 616, 1148). There appears to be an excess above 70 keV during the brightest parts of the peaks. However, since these spectra reach an intensity of 200 Crab, they are dominated by systematics, and the apparent excess may be an artifact of our calibration.
This behavior is qualitatively consistent with confined fireball models. The narrow peaks are optically thin fireballs, and the wide peaks are fireballs that are originally optically thick with contracting photospheres that reach transparency at the inflection point. Quantitative comparison to this model awaits more detailed calculation.
Light curves and lists of burst times for this activity may be viewed at http://gcn.gsfc.nasa.gov/gcn/other/SGR1900+14_swift_bat.html | 2006-04-04 06:24:00 | gamma ray,soft gamma-ray repeater | 2006-04-04 | 06:24:00 | 3,862 | [
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] | 788 |
790 | INTEGRAL discovery of two faint hard X-ray sources in the Galactic Bulge | M. Turler (ISDC, Geneva), S. E. Shaw (Southampton, UK/ ISDC, Geneva), E. Kuulkers (ESA/ESAC, Spain), S. Brandt, (DNSC, Denmark), T. J.-L. Courvoisier (ISDC, Geneva), A. Domingo Garau (LAEFF/INTA, Spain), K. Ebisawa (NASA/GSFC, USA), P. Kretschmar (ESA/ESAC, Spain), C. Markwardt (NASA/GSFC, USA), N. Mowlavi (ISDC, Geneva), T. Oosterbroek (ESA/ESTEC, Netherlands), A. Orr (ESA/ESTEC, Netherlands), A. Paizis (IASF, Milano), D. RÃsquez Oneca (LAEFF/INTA, Spain), C. Sanchez-Fernandez (ESA/ESAC, Spain), R. Wijnands (UvA, Netherlands) | Analysis of INTEGRAL Galactic Bulge monitoring observations (ATel #438) taken between 16:51 and 20:33 UTC on 3 April 2006, reveals the presence of two new sources of hard X-rays. They both have a detection significance exceeding 6 sigma in the IBIS/ISGRI 20-60 keV band with a corresponding flux of ~10 mCrab. The two sources are located close together, approximately 0.8 degrees apart.
Their characteristics are as follows:
Unfortunately the new source positions were situated just at the edge of the JEM-X field of view, where the sensitivity of the instrument is low, and hence the detections cannot be confirmed by this instrument.
RXTE PCA observations of the Galactic Center region on 1 April at 04:35 UTC and 4 April at 20:41 UTC place only upper limits on the 2-10 keV emission, of approximately 1 mCrab (systematics dominated). This could indicate that both sources are fast transients, or highly absorbed, if the INTEGRAL detections are confirmed.
More details of the analysis can be found at http://isdc.unige.ch/Science/BULGE
Further observations are encouraged. | 2006-04-06 23:32:00 | x-ray,transient | 2006-04-06 | 23:32:00 | 1,079 | [
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791 | XMM-Newton observation of XTE J1817-300 | G. Sala, J. Greiner (MPE Garching) | The black hole candidate XTE J1817-300 was observed for 20 ks with XMM-Newton on 13 March 2006, 45 days after the X-ray maximum as seen with RXTE/ASM. The EPIC-pn camera was used in the Burst mode and a simultaneous high resolution spectra was obtained by RGS1. Spectral fits have been performed using XSPEC. The EPIC-pn spectrum is dominated in the 1-6 keV range by a thermal disk with kT=0.74 keV, and a power law with photon index 3.3±0.1 at higher energies. We find NH=(2.6-2.8)x1021cm-2 and a flux of 8.6x10-9 erg/cm/s (0.4-10 keV). This corresponds to a luminosity of 1.0x1036 (d/1 kpc)2 erg/s. In the RGS spectrum, we detect the OI K-alpha interstellar absorption line at 527 eV, with equivalent width 1.36(+0.02/-0.01) eV. This value and the detected NH fits well in the OI K-alpha line vs NH correlation reported in Sala et al.(2006, submitted to A&A) using GRO J1655-40 XMM-Newton observations together with several sources found in the literature. The observed NH value is marginally larger than the average value in the source direction (Dickey & Lockman, 1990, ARAA, 28, 215). This locates XTE J1817-330 behind the galactic slab of ISM (adopted to be 150 pc), and provides a lower limit for the distance of 1.0 kpc. Recalling that the maximum flux detected during high/soft state by RXTE/ASM was ~2 Crab, and assuming the source was at 10% of the Eddington luminosity (as many other BH transients at maximum) at that time, we derive an upper limit of 4 kpc. Thus we estimate the distance to be in the range 1-4 kpc. | 2006-04-07 23:33:00 | x-ray,black hole,transient | 2006-04-07 | 23:33:00 | 1,529 | [
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] | 790 |
792 | Optical observations of Nova V2362 Cyg | K. Czart, M. Lewandowski, G. Maciejewski, T. Tomov, M. Mikolajewski, A. Niedzielski (Torun Centre for Astronomy, Torun, Poland) | We report on optical spectral observations and V brightness estimate obtained with 60/90 cm Schmidt-Cassegrain telescope and the SAVS camera of the Nicolaus Copernicus University Observatory in Piwnice.
The spectrum obtained on April 6.05 UT (3400-7050AA, resolution of 4A) shows numerous absorption lines (HI, FeII, CaII among the others) and in the range between H-delta and H9 resembles typical A5-A7 supergiant photosphere. The only emission seen in the spectrum is P-Cygni component of H-alpha (intensity of 1.2 relative to continuum, RV=-55 km/s with absorption component at RV=-680 km/s). The other hydrogen lines (H-beta to H12) appear in absorption only and have mean RV of -550 km/s. Similar RV show the absorptions of ionized metals such as FeII and CaII (-595 km/s).
On Apr. 7.05 UT an estimate of V=8.80 mag was obtained with the SAVS camera (Niedzielski et al.2003 AcA 53, 281). In the spectra of April 7.10 UT (3750-4750AA and 5750-6750AA, resolution of 2 A) all HI lines from H-alpha to H8 are seen in emission and show weak absorption components. Also present are wide blends of NII 6168A + OI 6157A and probably 74rd multiplet of FeII (6148A, 6238A and 6456A) seen as emissions with weak absorption components. H-alpha emission is the strongest line (intensity of 2.5 relative to continuum, RV=-110 km/s, FWHM about 1850 km/s) and shows clearly presence of two absorption components: one at -770 km/s, and second at -1750 km/s. HeI 5876 is now present in absorption and has two components with RV of -800 and -1700 km/s.
The spectra of April 8.06 UT (4050-5050AA and 5720-6720AA, resolution 2A) are very similar to those of April 7.10. H-alpha emission component intensity is 3.2 times continuum, H-beta 2.5. The absorption components of H-alpha show RV of -800 and -1795 km/s (in H-beta the RV of absorption components is -882 and -1733 km/s respectively). The mean RV of the absorption components of other lines present in the spectrum is -880 and -1730 km/s. The NaI D1 and D2 interstellar lines are clearly resolved in the spectra with a mean equivalent with about 0.8 A corresponding to a distance of about 1.5 kpc (Allen 1973, Astrophysical Quantities). | 2006-04-10 13:21:00 | optical,cataclysmic variable,nova,star,variables | 2006-04-10 | 13:21:00 | 2,180 | [
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] | 791 |
793 | Swift Observations of SN 2006bp in NGC 3953 | S. Immler, Goddard Space Flight Center, NASA, and Universities Space Research Association; P. J. Brown, Pennsylvania State University, and P. Milne (Steward Observatory, University of Arizona) on behalf of the Swift-satellite team | We report on Swift Ultraviolet/Optical Telescope (UVOT) and X-Ray Telescope (XRT) observations of SN 2006bp (cf. CBET #470) obtained on Apr. 10.54 UT.
We confirm the detection of a new object at R.A. = 11h53m55s.70, Decl. = +52o21'10".4 (equinox 2000.0) as compared to Digitized Sky Survey images, consistent with the position reported by Nakano on CBET #470, with UVOT magnitudes V = 15.5, B = 15.8, U = 14.7, UVW1 [181-321 nm] = 14.8, UVM2 [166-268 nm] 15.2, and UVW2 [112-264 nm] = 14.9. Statistical and systematic errors are 0.1 mag each.
Comparing the B-V and U-B colors with other supernovae from Poznanski et al. (2002, PASP 114, 833) shows that 2006bp is a young type-II SN.
An excess of X-ray counts is detected from the position of the SN at a 2.0-sigma level in the 3.4 ks XRT data obtained simultaneously. The XRT net count rate of (1.7+/-0.9)E-03 cts/s corresponds to a (0.2-10 keV) X-ray flux and luminosity of (9.0+/-0.5)E-14 ergs/cm/cm/s and (2.4+/-1.3)E39 ergs/s, respectively, for an adopted thermal plasma spectrum with a temperature of kT=10 keV and a distance of 14.9 Mpc.
Further Swift observations are scheduled. | 2006-04-11 04:30:00 | optical,x-ray,supernovae | 2006-04-11 | 04:30:00 | 1,139 | [
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] | 792 |
794 | SGR-like Burst from Direction of AXP 4U 0142+61 | Victoria Kaspi, Rim Dib (McGill University), Fotis Gavriil (NASA/GSFC) | On MJD 53831.3 (April 6, 2006) during regular RXTE/PCA monitoring of AXP 4U 0142+61, we detected a single small SGR-like burst. The burst is similar to the smallest burst seen from AXP 1E 1048-5937, lasting approximately 1.8 s and having total fluence approximately 100 counts in the 2-20 keV band, with 3 operational PCUs. Optical/IR observations of the source and its putative debris disk may be warranted. We regret the delay in posting this telegram. | 2006-04-14 18:39:00 | far-infra-red,infra-red,optical,x-ray,gamma ray,neutron star,pulsar,soft gamma-ray repeater,star,transient,request for observations | 2006-04-14 | 18:39:00 | 454 | [
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] | 793 |
795 | The progenitor of Nova Cygni 2006 (=V2362 Cyg) | D. Steeghs (CfA), R. Greimel (ING), J. Drew (Imperial College London), M. Irwin (IoA), B. Gaensicke (Warwick), P. Groot (Nijmegen), C. Knigge (Southampton) and the IPHAS collaboration | We report on the detection of the likely progenitor to Nova Cygni 2006 = V2362 Cyg (IAUC # 8697 , # 8698 , ATel #792) using images from the INT Photometric H-Alpha Survey (IPHAS; http://www.iphas.org ).
The field containing the classical nova was observed as part of our galactic plane survey on Aug. 3rd 2004 between 02:58-3:42UT using the Isaac Newton Telescope at La Palma Observatory. No clouds were present and seeing was stable, delivering a 1" image-quality sampled with 0.33" per CCD pixel. The images were calibrated using photometric standard star observations.
A single point source was detected at the position reported in IAUC # 8702 with broad-band magnitudes of r'=20.3 +/- 0.05, i'=19.76 +/- 0.07. Our two narrow-band Halpha exposures suggest a r'-Halpha color index of 0.6-0.8 on the Vega scale. Comparing its r'-i' and r'-Halpha colors with the main-sequence locus defined by the large number of field stars in our images places it well above the main-sequence, implying line emission in the Halpha passband. A r'=14.8 star sits 5" west, but has completely different colors such that the apparent Halpha emission cannot be caused by contamination from this nearby star.
The total galactic extinction along the line of sight amounts to E(B-V)=0.8 (from Schlegel et al. (1998) dust-maps as well as our own field star photometry), while outburst spectroscopy indicates E(B-V)=0.56 (IAUC # 8702 ). Our IPHAS colors are consistent with an optically thick accretion disk spectrum reddened to E(B-V)=0.65 +/-0.05, corresponding to an Halpha EW of 40 +/- 15 (see also Drew et al. 2005, MNRAS 362, 752). These properties all fit well with a classical nova progenitor identification and we thus propose this to be the quiescent counterpart to V2362 Cyg.
Our quiescent colors imply an outburst amplitude of ~12 magnitudes, and assuming a typical M(V)=3-5 for a pre-nova cataclysmic variable accreting at high rates would place the system at 5-12 kpc. | 2006-04-15 08:54:00 | optical,binary,cataclysmic variable,nova,star,transient,variables | 2006-04-15 | 08:54:00 | 1,961 | [
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796 | INTEGRAL detection of a strong outburst in 4U 1954+31 | S. Paltani (ISDC, Geneva), D. Attie (CEA, Saclay), A. Domingo Garau (LAEFF, Madrid), S. Larsson (Stockholm Observatory), J. Paul (CEA, Saclay), P. Shtykovsky (SRI, Moscow), A. Strong (MPI, Garching), O. R.Williams (ISOC/ESAC, Madrid) | We report the dectection of a ~150 mCrab outburst in the transient high mass X-ray binary 4U 1954+31, observed in the Galactic Plane Survey (GPS) by INTEGRAL. The flux in the IBIS/ISGRI instrument reached 17.7 counts/s (165 mCrab, 32-sigma detection) in the 20-40 keV band. The observations started at 00:14 UTC on Apr 15, 2006. The flux was already ~15 counts/s (140 mcrab). It peaked 40 min later, and then fell to about 10 counts/s (95 mcrab). The source was not detected anymore in the pointing starting two hours after the first detection; as the source was well off-axis, this gives an upper limit of about 4 counts/s (35 mCrab). 4U 1954+31 is also detected in the 40-80 keV band, with a flux of 3.4 counts/s (55 mCrab). The significance is about 6 sigmas. Unfortunately, 4U 1954+31 does not cross the field of view of Jem-X during this GPS scan. This is the first detection of this source in ISGRI, although its location in the Galactic Plane and close to Cyg X-1 makes that it has been observed a large number of times. The source is also not present in the 2nd IBIS/ISGRI catalogue (Bird et al., 2006, ApJ 636, 765). Inspection of the R-XTE ASM light curve shows that the source is regularly detected and that bursts of the order of 50 mCrab in the 2-10 keV band occur 2-3 times per year, lasting a few days. These bursts usually occur during long periods (~a year) of increased activity. 4U 1954+31 will be reobserved in the GPS on Apr 24. | 2006-04-16 20:17:00 | x-ray,gamma ray,binary,transient | 2006-04-16 | 20:17:00 | 1,449 | [
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797 | Swift/BAT Detection of a 5 hour Period in 4U 1954+31 | R. Corbet (GSFC/USRA), L. Barbier (GSFC), S. Barthelmy (GSFC), J. Cummings (GSFC/NRC), E. Fenimore (LANL), N. Gehrels (GSFC), D. Hullinger (UMD), H. Krimm (GSFC/USRA), C. Markwardt (GSFC/UMD), D. Palmer (LANL), A. Parsons (GSFC), T. Sakamoto (GSFC/NRC), G. Sato (ISAS), J. Tueller (GSFC), on behalf of the Swift-Survey team | The power spectrum of the Swift Burst Alert Telescope (BAT) light curve of 4U 1954+31 obtained between 2004 December 11 and 2005 September 20 shows, in addition to low frequency noise, modulation at a period of approximately 5.09 hours. The peak in the power spectrum near 5 hours shows a complex structure. When the light curve is examined on shorter time scales it is seen that during the course of the BAT observations the period changed from approximately 5.19 to 5.02 hours in a near monotonic fashion. The mean count BAT count rate from 4U 1954+31 in the range 14 - 195 keV is 12.7 (+/- 0.2 statistical) E-4 counts/s/fully illuminated detector (where the area of a single BAT detector is 0.16 cm^2) which corresponds to 28 mCrab. The Fourier modulation amplitude at 5 hours is approximately 6.5 E-4 counts/s/detector.
The large change in the 5 hour period makes it implausible that it is caused by orbital modulation. Masetti et al. (2006, astro-ph/0603227) also determine the optical counterpart of 4U 1954+31 to be an M 4-5 giant which would imply a very long orbital period in order for the star not to overfill its Roche lobe (cf. the Porb > 100 days constraint for GX 1+4 where the donor is an M5 III star, Chakrabarty & Roche, 1997, ApJ, 489, 254). In addition, the period change is too large for the it to come from the rotation period of an accreting white dwarf because of the large moment of inertia of these objects.
The 5 hour period is somewhat reminiscent of the 2.7 hour period seen in the high-mass X-ray binary 2S 0114+650 which is believed to be a neutron star rotation period (e.g. Farrell, Sood, & O'Neill, 2006, MNRAS, 367, 1457 and references therein). If the periodicity in 4U 1954+31 does indeed represent the rotation period of a neutron star, then the rapid spin-up requires an X-ray luminosity of approximately 5 E35 ergs/s (e.g. Joss & Rappaport, 1984, ARAA, 22, 537). In order to reconcile this luminosity with the observed X-ray flux and the upper limit on the distance to 4U 1954+319 of 1.7 kpc derived by Masetti et al. (2006) a high degree of absorption of the X-ray spectrum is required.
Alternatively, the 5 hour modulation might be caused by some type of instability in an accretion disk or magnetosphere similar to the cause of the 3.96 hour quasi-periodic flares observed on one occasion from EXO 2030+375 (Parmar et al. 1989, ApJ, 338, 359). An explanation of the period as a pulsation in the mass donor appears problematic as the fundamental pulsation periods of M giants are very long and there is little evidence for pulsations on periods less than 10 days (Koen, Laney, & van Wyk, 2002, MNRAS, 335, 223). | 2006-04-21 00:27:00 | optical,x-ray,binary,neutron star,pulsar,star,transient,variables | 2006-04-21 | 00:27:00 | 2,656 | [
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798 | Discovery of radio emission from X-ray pulsar XDINS 1RXS J214303.7+065419+06 | V. M.Malofeev (PRAO LPI, Pushchino), O. I. Malov (PRAO LPI, Pushchino), D. A. Teplykh (PRAO LPI, Pushchino), S. V. Logvinenko(PRAO LPI, Pushchino), I. I. Litvinov (PRAO LPI, Pushchino), S. B. Popov (SAI MSU, Moscow) | We report the detection of radio pulses from X-ray pulsar 1RXS J214303.7+065419 at the frequency 111.23 MHz. The pulsed X-ray emission with the spin period 9.437 s was discovered in March 2005 by Zane et al. (astro-ph/0503239) towards the dim isolated neutron star (XDINS) RBS 1774 using XMM-Newton observations. Our observations were made during 66 days in October-March 2005-2006 on the Large Phased Array at Pushchino Radio Astronomy Observatory (PRAO, Russia), sensitive transit radio telescope consisting of 16384 dipoles and operating at the frequency 110.5 +/- 1.5 MHz. We use multi-channel receiver with 64 channels, where each individual channel has a width equal to 20 kHz. Pulsar signal (S/N>4) was detected in a one third of days with the integration of 20 pulses for each day. We obtained the estimation of the flux density 60+/-25 mJy. This pulsar demonstrates a complex form of the integration profile (possible there are three components) and the width of the integration profile at 50 percent of the intensity maximum is 990 ms, that is about four times less than in X-rays. There is irregular interpulse at the phase ~1/2 of period. The estimate for the dispersion measure 8+/-5 pc/cm^{3} places the pulsar at the distance ~400 pc, according to the measurements of the distances of a few surrounding pulsars (Taylor et al. 1995, unpublished data). Our distance is close to the estimate 280 pc obtained by Zane et al., 2005. We derive the period of 9.43707(10) s, and the estimate period derivative is (-1.5+/-2.2)x10^{-12} s/s on JD 2453680.0 using reliable measurements (for 10 days of observations) between JD 2453661 and JD 2453711. This is the second case of the radio emission discovery for the XDINS. The 10.31 s X-ray pulsar 1RXS J130848.6+212708 (RBS 1223) was detected by Malofeev et al. (IAU Symp. 218, ASP Conf. Ser., p. 261, 2004; Astron Rep. 49, 242, 2005). The radio emission detection is very important, because there is no model for radio emission of such pulsars. | 2006-04-21 15:46:00 | radio,x-ray,neutron star,pulsar,star | 2006-04-21 | 15:46:00 | 1,998 | [
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] | 797 |
799 | Swift/BAT detection of a new X-ray source, SWIFT J1656.3-3302, in the Galactic Center region | T. Okajima (JHU/NASA/GSFC), J. Tueller (NASA/GSFC), C. Markwardt (UMD/NASA/GSFC), M. Ajello (MPE Garching), V. Beckmann (UMBC/NASA/GSFC), T. Belloni (INAF/OAB), A. Falcone (PSU), O. Godet (U Leicester) , D. Grupe (PSU), S. Holland (USRA/NASA/GSFC), J. Kennea (PSU), K. Mukai (USRA/NASA/GSFC), R. Mushotzky (NASA/GSFC), R. Sambruna (NASA/GSFC) | We report the detection of unidentified source SWIFT J1656.3-3302, which is located at RA = 254.08, Dec = -33.03 (J2000), galactic coordinates l = 350.60, b = 6.36. The source was detected at 5.7 sigma significance during the Swift/BAT hard X-ray survey (mid Dec. 2004 to mid Sept. 2005). The BAT spectrum (14-200 keV) is very hard with a photon index of 1.26 +/- 0.3. The flux is 1.0E-10 ergs/cm^2/sec. In the Galactic Center, the risk of source confusion is significant. Due to a small excess in the 14-25 keV band next to this source, we have expanded our error radius to 12 arcmin from the nominal value of 6. No counterpart has yet been identified, but Swift/XRT observations are planned. Based on our analysis of the INTEGRAL IBIS/ISGRI public data, the source is marginally detected at a much lower flux of ~6E-12 ergs/cm^2/sec. (Total on-source exposure is 2.6 Ms between 02/28/2003 and 10/20/2004.) Correcting to the same energy band, the source increased in brightness by more than a factor of 4 between the two observations. | 2006-04-28 04:41:00 | x-ray,transient,request for observations | 2006-04-28 | 04:41:00 | 1,035 | [
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] | 798 |
800 | IGR J19140+0951 simultaneously observed with INTEGRAL, Swift and RXTE | J. Rodriguez (CEA/AIM Saclay, France), V. Beckmann (NASA/GSFC/UMBC, USA), D. C Hannikainen (Obs. of Helsinki, Finland), F. Lebrun (CEA/APC, France), S. E. Shaw (Univ. of Southampton, UK), D. Willis (MPE Garching, Germany) | The INTEGRAL source IGR J19140+0951 (Hannikainen et al. 2004, A&A, 423, L17) has been simultaneously targeted with INTEGRAL, Swift, and RXTE on April 26-27 2006, for 21, ~7, and ~7 ks respectively. | 2006-04-28 22:19:00 | x-ray,gamma ray,black hole,neutron star,pulsar,star,transient | 2006-04-28 | 22:19:00 | 197 | [
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