cometadata/datacite-titles-descriptions-related-identifiers huggingface dataset:
DOI: 10.57780/esa-qyji547
title: 1570006

description: MAXI J1820+070 is a transient black hole X-ray binary (BHXRB) discovered by MAXI on March 11 2018. This outburst detected at almost any wavelength due to the low obscuration of the system is been monitored intensively by the astronomical community and so far has given rise to ~20 Astronomical Telegrams.Similarly to V404 Cyg the source displays intense flaring activity at almost any wavelength. But contrary to the highly absorbed V404 Cyg MAXI J1820+070 is an ideal candidate to understand the correlations between variability across the electromagnetic spectrum and therefore put stronger constraints in the relations between the physical phenomena producing emission in the different energy ranges and to study their variations on the different accretion regimes.The rise of the outburst has been monitored by INTEGRAL since March 16th 2018. Unfortunately the ongoing program will end by March 31st 2018. With this request and as a service to the community we propose to continue monitoring MAXI J1820+070 every single revolution with a 50 ksec exposure. With the current source flux around 3 Crab this will allow the generation of X-ray spectra of good enough S/N to characterise the system high energy emission and monitor variations of its slope indicative of spectral changes. As the source is not heavily absorbed in soft X-rays we request the observations to be performed in an HEX pattern in order to obtain continuous coverage with JEMX and be able to monitor as well variations in its soft X-ray emission.When the source flux decays below 50mCrab we propose to double the exposure to 100mCrab. We propose to continue this plan until the source reaches the quiescent state which we expect to happen in about 3 weeks.We will be in close communication with ISOC to provide feedback on the source flux so that the observing strategy can be modified when necessary. [truncated! Please see actual data for full text]
DOI: 10.57780/esa-r04hnfi
title: 1420031

description: As a follow-up of our earlier observations (2 Ms in AO-1 2.5 Ms in AO-2 and 2 Ms in AO-3) we propose a new deep 1.6 Msec exposure of the Galactic Center field which corresponds to 15% share time in the total available for this target in AO-14. Observations of the GC region make the best use of the unique INTEGRAL capabilities and undoubtedly are the most efficient investment of its precious observing time. It is important for the study of Galactic diffuse nuclear and positron annihilation lines however the main objectives of the proposed observations are the monitoring of Sgr A* and a dozen of black-hole and other peculiar X-ray binaries and search for the new transient sources and phenomena. [truncated! Please see actual data for full text]
DOI: 10.57780/esa-r420zly
title: 8860250

description: Crab 2012: SPI/IBIS 5x5 wide rev 1159-1160
DOI: 10.57780/esa-r4rexa3
title: 8860098

description: Crab 5*5 2006 SpringStandard Raster for SPI  and  IBIS
DOI: 10.57780/esa-r5kz7xy
title: 0620065

description: 3C 454.3 is one of the most variable blazars from radio up to gamma-raysenergy bands. In 2005 and 2007 the source was detected in a strong optical activity thattriggered observations by other observatories. In 2005 a strong hard X-rays emission was detected by INTEGRAL from 3 up to 200 keV the flux being afactor 2-3 higher than that previously observed. The model predictions were notstrongly constrained. The lack of gamma-rays data did not help to break thedegeneracy among the parameters in SSC and EC models. In 2007 the increase in the optical activity triggered Swift and AGILEobservations. During this flare AGILE detected a flux of 3C 454.3  that was the highest everdetected for this blazar (280+-40  E-8 photons cm ^-2 s^-1). On the other hand Swift-BAT did not detect a significant hard-X rays emission. At moment the available data do not help to  investigate the correlation (if any) between the hard-Xrays and gamma-rays emissions in both high and low gamma-ray activity.  AGILE is showing as 3C 454.3 is very active in the gamma-rays then the highstate seems to be the ``ordinary life of this source. However  we argue as all gamma-ray states of the source have to beinvestigated simultaneously with its hard-X rays state. On the basis of these considerations we request to monitor the activity ofthis blazar over a period of 1-week during the 3/4 weeks of a standard AGILE pointing. [truncated! Please see actual data for full text]
DOI: 10.57780/esa-r71kf76
title: 1020010

description: We ask for a two year INTEGRAL Key Programme to observe the area of the Galaxy bounded by  20   l   +20 and  15   b   +15 with a total of 2 Msec of observations per AO. The aim is to study the inner region of the Galaxy namely to continue the search for evidence for gamma-ray  ares from Sgr A   to continue measuring the  ux evolution of Sgr B2 through 2012 to monitor bursts and  ares from the many LMXB neutron star sources and to enable signi cant serendipitous science in the Galactic center region. [truncated! Please see actual data for full text]
DOI: 10.57780/esa-r8wn8q5
title: 8860394

description: SAS Calibration for rev. 2283
DOI: 10.57780/esa-r9ulyaq
title: 0399922

description: Scutum arm Proposal for AO 03 Cycle 2
DOI: 10.57780/esa-rcc2ktu
title: 8860357

description: Crab Calibration 2017.2 (1856-57): IBIS/SPI
DOI: 10.34810/data57/1
title: RNA and protein WAT content.tab
DOI: 10.34810/data57/2
title: Enzyme Activities PG WAT.xls
DOI: 10.34810/data57/3
title: Enzyme Activities ME WAT.xls
DOI: 10.34810/data57/4
title: Enzyme activities SC WAT.xls
DOI: 10.34810/data57/5
title: PCR Results.xls
DOI: 10.34810/data57/6
title: Enzyme Activities RP WAT.tab
DOI: 10.57780/esa-rducfcw
title: 0920014

description: The nature of ultraluminous X-ray sources (ULXs) remains unknown. We do not know whether they host stellar- or intermediate-mass black holes nor do we have a clear understanding of the accretion process. Similarly poorly studied is accretion onto supermassive black holes in low-luminosity active galactic nuclei (LLAGN). To address these problems high-sensitivity observations at energies above 10 keV are needed. We propose to add 2+2 Ms of exposure with INTEGRAL in AO9 and AO10 to a 4 Ms    exposure to be accumulated in AO7 and AO8 in a unique field where two of the brightest ULXs M82 X-1 and Holmberg IX X-1 and one of the brightest LLAGN M81 are located. We will measure the spectra of these sources in the 3-100 keV energy band and study their spectral variability. A preliminary analysis of ~2.5 Ms of observations provided to us so far confirms the feasibility of achieving our scientific goals. [truncated! Please see actual data for full text]
DOI: 10.57780/esa-rekzq9k
title: 0299922

description: Galactic Centre Deep Exposure for AO 02 and Pattern 22 Cycle 2
DOI: 10.57780/esa-retnp2w
title: 8860093

description: This is a public observation where the Earth will drift through the field of view of the INTEGRAL instruments. Results from this observation will help in separating the cosmic and instrumental backgrounds and so ultimately lead to improved background subtraction.Scientifically the main goals are to measure the spectral shape of the cosmic X-ray background emission above 20 keV and to study any high-energy emission from the Earth during storms in auroral regions. [truncated! Please see actual data for full text]
DOI: 10.57780/esa-rgazgd0
title: 0740026

description: Even though the spectrum of canonical hard state of Galactic black hole transients (GBHT) is often described by a power  law with a cut-off analysis of the RXTE and the INTEGRAL data show that this description may not be entirely correct. Some sources show a break in the power-law spectrum during the transition to the hard state but once a compact jet forms the break disappears at the HEXTE band (15 -- 200 keV). Therefore the shape of the hard X-ray spectrum in the low hard state is still one of the most important open questions of the black hole science. The disappearance of cut-offs may point out yet another relation between the  jets and high energy emission. We propose one TOO observation of a GBHT with INTEGRAL at the hard state after the jet turns on (determined by radio or optical/infrared OIR observations) to search for breaks beyond 200 keV. By characterizing the gamma-ray domain at the hard state we will constrain the X- and gamma-ray emission mechanisms and also investigate the relation between the X-ray emission and jet formation. We will achieve multiwavelength coverage using ATCA in radio and SMARTS in optical/infrared. The current archival data are not enough to carry out this research. We request a single observation of  300 ks for one source. [truncated! Please see actual data for full text]
DOI: 10.57780/esa-rhk4y7z
title: 8860326

description: OMC FF sequence ISOC V10 onwards: sequence of ff measurements with LED on/off followed by a DC cal.
DOI: 10.57780/esa-rhrmsca
title: 1420016

description: Massive stars and their impacts on their surrounding interstellar medium comprise the feedback scenario which is one of the main astrophysical issues in the context of galaxy and cosmic chemical evolution. Radioactivity from 26Al adds a unique diagnostic tool for studying this scenario in nearby massive-star regions. The Orion region hosts one of the closest such regions at ~400 pc. COMPTELs measurement of 1809 keV emission from this region had shown an interesting offset of the 26Al emission source from its likely sources and emission appears rather extended. This suggests champagne-like outflow into the Eridanus cavity as has recently also been seen with XMM-Newton. If true this opens unique possibilities to study the ISM as it is shaped by massive stars and the interaction of massive stars with their surrounding ISM in a new way: Due to their proximity and location on the near side of molecular clouds and at the edge of a large cavity we can compare the locations of massive stars to the morphology of the ISM and the emission pattern of 26Al radioactivity in order to constrain 26Al ejection from massive stars in mass and velocity. Previous observations led to ~3 Ms of exposure merely enough for a marginal hint of the expected signal. With our proposed deepening of exposure we aim to measure the intensity and kinematics of this nearby 26Al source with INTEGRAL. With these observations we can also search for annihilation radiation and for the intensity of nuclear deexcitation gamma-rays in the MeV range both valuable diagnostics of the structure of superbubble interiors and more than 30 Fermi sources are within our target region. But mainly this will give us unique measurements of ISM dynamics and massive stars as its driving engines within INTEGRALs lifetime  there is hardly a more suitable and closer target region. [truncated! Please see actual data for full text]
DOI: 10.57780/esa-rhza3dv
title: 0820027

description: The SNR RX J1713.7-3946 is part of a class of remnants dominated by synchrotron emission in X-rays and is one of the few  detected at the TeV. It is therefore an excellent target to study particle acceleration at SNR shocks. The nature of the particles producing TeV emission is still a matter of controversy. The strong similarities between X-ray and TeV images suggest a leptonic origin but the required magnetic field is quite low. On the other hand to be viable hadronic scenarios require high ambient matter density at odds the the absence of  strong thermal X-ray emission. The hard X-rays probe the electrons in the spectral cutoffs region and are therefore fundamental to understand the mechanisms of acceleration to the highest energies. Suzaku has been able to measure the integrated spectrum of the remnant but so far no detailed spectro-imagery exist for this object. In the previous AO we proposed a 4 Ms observation of RX J1713.7-3946 to map the hard X-ray emission from the remnant from 10 keV up to 50 keV and to resolve spatially the hard X-ray spectrum of the remnant. 2 Ms will be taken in 2010. We propose here to complete this observation with 2 Ms taken in hexagonal dithering pattern to provide also a good coverage with Jem-X. This will allow a mapping of the spectral cutoffs in the shell and hopefully shed some light on the long standing problem of the origin of cosmic rays up to the knee. [truncated! Please see actual data for full text]
DOI: 10.57780/esa-ritmrxq
title: 0620054

description: We ask for four 90 ks long observations of the high mass X-ray binary 4U 1907+09 spread out over INTEGRALs AO6. The source shows a rich phenomenology and might be a missing link with respect to Supergiant Fast X-ray Transients. The observations will allow us to study the dip/non-dip duty cycle of the source. They will represent one of the best data sets to date to test our newly developed physical models for cyclotron lines for a moderately bright source since 4U 1907+09 is persistent (although dipping and flaring) and shows two lines. Also after almost 20 years of continuous spin down 4U 1907+09 was recently discovered by our team to have undergone a torque reversal episode and is now spinning up. This type of behavior is very rare and monitoring the pulse period evolution now provides a unique opportunity to constrain models for the torquing of the neutron star by the accreted material. [truncated! Please see actual data for full text]
DOI: 10.57780/esa-rkc9nb4
title: 8860019

description: This Crab onaxis staring observation is used to determine the  imaging properties of IBIS and to provide an absolute calibration of IBIS up to 2 MeV.
DOI: 10.57780/esa-rkq6g8f
title: 2020018

description: Fast Radio Bursts (FRBs) have already provided a large wealth of interest and speculation about their origin complemented by a large number of applications for new science that can be explored once we have a statistically significant sample of them. FRBs show an impulsive behaviour characterised by a $sim$ms-long very energetic burst. A growing subset of the population is now characterised by repeating bursts. The chance to observe FRBs more than once has helped constrain their properties and shaped the proposed models for their origin. The identification of its host galaxy has allowed in-depth studies of the original repeater: FRB 121102. Amongst the new repeaters FRB 180916.J0158+65 has the lowest projected dispersion measure and was most recently localised to a nearby massive spiral galaxy. Its high activity led most recently to the discovery of a 5-day activity cycle of the source every $sim 16$ days. With its closeness its localisation and now its periodicity FRB 180916.J0158+65 represents the most promising candidate for investigating the properties of repeaters which have so far been elusive in the case of FRB 121102. One outstanding question concerns the multi-wavelength emission from FRBs which are at present only seen in the radio band. Higher energy bursts are predicted by most FRB models either simultaneously with the radio bursts or as an afterglow after the bursts. We propose INTEGRAL observations combined to a capillary international multi-wavelength campaign led by the Sardinia Radio Telescope with the aim of detecting for the first time this source at hard X-rays and collecting unprecedented observational information about the broadband emission properties of the source and in turn discriminating its nature. [truncated! Please see actual data for full text]
DOI: 10.57780/esa-rosfau2
title: 1540008

description: There is good evidence that Anomalous X-ray Pulsars (AXPs) and Soft Gamma Repeaters (SGRs) are magnetars objects in which the magnetic field energy dominates all other energy sources including rotation. This implies that they possess the strongest known magnetic fields in the universe (10^13-15 G). Magnetars go through phases of intense activity during which they may emit a few up to hundreds of bursts within a period of weeks to months and at the same time they can increase their persistent flux by more than two orders of magnitude.  During those periods they exhibit properties which are quite different from those in quiescence. Their strong magnetic fields are probably mainly responsible for these changes and accordingly it is interesting to study them intensively at those times. In addition the discovery of transient magnetars has opened a new perspective in the field.  This proposal is aimed at gathering new insights on the physics of magnetars through the study of the multi-band spectrum of the initial phase of their outbursts. We request four 200 ks ToO INTEGRAL and 20 ks of coordinated Swift/XRT observations to be triggered by an X-ray flux increase or burst activation from known and new magnetars. [truncated! Please see actual data for full text]
DOI: 10.57780/esa-rrmhx3s
title: 0220151

description: It has been known for many years that the X-ray spectral indices ofSeyfert galaxies in the 2-10 keV band become steeper as the fluxincreases. Recently we and others have defined the shape of theflux/spectral index relationship very precisely and in particular itis noted that the spectral index reaches an asymptotic level at highfluxes.There are two main possible explanations for this relationship.  Thefirst possibility is that the spectrum could consist of twocomponents a relatively hard component of approximately constantflux and a soft component of variable flux.  The second possibilityis that there is intrinsic spectral variability in the component whichdominates the X-ray flux such that the spectrum does becomeintrinsically softer at high fluxes perhaps pivoting about some highenergy (100keV).Determining which possibility is actually the case has importantimplications for the physics of the high energy emission regionand is the main aim of the present proposal. Integral is ideallysuited to this programme. [truncated! Please see actual data for full text]
DOI: 10.57780/esa-rs0y3fc
title: 1870005

description: INTEGRAL TOO observattions of  4U1636-536
DOI: 10.57780/esa-rs6ujk8
title: 0320013

description: Recently we published the first all-sky map at 511 keV (Knoedlseder et al. 2004) which clearly showed that the positron annihilation radiation from our galaxy is concentrated around the galactic center. The observed emission could not be unambiguously decomposed into bulge halo and disk components. We propose to resolve the ambiguity concerning a halo component by observing at intermediate latitudes (b=+/-25deg) North and South of the galactic center for 2*10^6 s each. Any 511 keV line emission from these regions is dominated by the halo component. The proposed observations are therefore ideally suited to establish the existence of or to setstringent limits on a galactic halo component. The existence or non-existence of a halo component has far-reaching implications for the annihilation rate and the origin of positrons in our galaxy in general and in the bulge and disk in particular. Possible halo positron sources are members of the old stellar population (such asType~Ia supernovae novae or low-mass X-ray binaries) or light dark matter. [truncated! Please see actual data for full text]
DOI: 10.57780/esa-rsq4kqj
title: 0629700

description: This is an artificial proposal
DOI: 10.57780/esa-rtayz63
title: 0820030

description: The nature of ultraluminous X-ray sources (ULXs) remains controversial. We do not know whether they host stellar- or intermediate-mass black holes nor do we have a clear understanding of the accretion process. Similarly poorly studied is the accretion onto supermassive black holes in low-luminosity active galactic nuclei (LLAGN). To address these problems sensitive observations at energies above 10 keV are needed. We propose to observe with INTEGRAL for a total exposure of 4 Msec (2 Msec in AO7 + 2 Msec in AO8) a unique sky region where two of the brightest ULXs M82 X-1 and Holmberg IX X-1 and one of the brightest LLAGN M81 are located. We will measure the spectra of these sources from 3 keV up to 50--100 keV and possibly study their spectral variability. At the time of this writing ~1.5 out of the 2 Msec of observations granted in AO7 have been provided to us. A preliminary analysis of these data confirms the feasibility of achieving our scientific goals upon completion of the entire observational campaign. [truncated! Please see actual data for full text]
DOI: 10.57780/esa-ru1inr8
title: 0299802

description: Galactic Plane Survey for AO 02 and Pattern 02
DOI: 10.57780/esa-rwexikm
title: 0420034

description: We propose to continue the monitoring of  GRS 1915+105 and its surroundings during AO4 with a strategy somewhat different than the ones we previously adopted hence with slightly different scientific goals. Instead of having 100 ks pointings (which allowed us to explore the high energies) we want 20 ks pointings in order to  understand the origin of its high variability and to probe the hierarchichal evolution between classes they should be taken every second revolution. We will finally obtain time resolved spectra of all states.  The simultaneous use of JEM-X in the soft X-rays IBIS and SPI in the soft Gamma-rays will enable us to study the origin of the spectral transitions giving birth to a particular class of variability. We aim at studying the interplay between the soft and hard X-ray components the different time scales of their variations in relation with different physical models and the tight connection between the accretion and ejection processes. For this purpose we will provide simultaneous radio (Ryle VLA GMRT Nancay) and infrared (Sierra NevadaESO) observations.  IBIS and JEM-X are  the prime instruments for this study. Although GRS 1915+105 is the main target of our study we outline here that amongst the ~10 sources usuallyobserved in this field our team aims at studying a handful of them with particular interest on IGR J19140+0951 (which is always in the totally coded field of view of IBIS and detectable with JEM-X) with the view to study its spectral behaviour/evolution (along its known orbit) and survey Ser X-1 Aql X-1 XTE J1908+094 (in the TCFOV) the latter 2 are transient and monitor their X-ray evolution along a possible outburst. For these particular sources multi-wavelength observations will also be conducted. We request that our observations be undertaken in segments of 20 ks exposures during the entire visibility period of 6 months once every second revolution hence 30 po [truncated! Please see actual data for full text]
DOI: 10.57780/esa-rwu8u9x
title: 1220016

description: We propose to continue our Key Programme that consists of high-cadence monitoring of the inner spiral arms of the Galaxy with INTEGRAL paired with ToO observations of new transients with XMM-Newton and Swift. The INTEGRAL Spiral Arms (ISA) program (25.6 ks per spacecraft revolution during visibility periods for a total of 1.2 Ms) complements the successful Galactic Bulge (GB) program by extending the monitored region of the Galaxy to the Inner Perseus/Norma Arm tangents on one side of the GB and the Scutum/Sagittarius Arms on the other. These fields feature a high density of obscured high-mass X-ray binaries (HMXBs) including Supergiant Fast X-ray Transients (SFXTs) as well as other hard X-ray emitting sources (e.g. microquasars low-mass X-ray binaries and magnetars) that INTEGRAL is well-suited to finding thanks to its large field of view and angular resolution at high energies even in crowded regions of the sky. Mosaic images and source light curves in 2 energy bands for ISGRI and JEM-X are being provided to the community (http://isa.gcsu.edu) permitting rapid dissemination of results which enable prompt follow-up of interesting events. The ISA project represents the cornerstone of our ongoing study of transient and variable hard X-ray populations in the Milky Way. [truncated! Please see actual data for full text]