cometadata/datacite-titles-descriptions-related-identifiers huggingface dataset:
DOI: 10.57780/esa-1258h3g
title: 1520009

description: We propose to continue the renewed INTEGRAL-multiwavelengh monitoring of GRS 1915+105 with the goal to understand the tight connections that exist between the different emitting media and placed in a broader context understand accreting-ejecting sources in general. As for AO 14 we will take advantage of new facilities (the Sardinia radio telescope in the radio domain and NICER at soft X-rays) while tentatively increasing the number of wavelengths covered by including infrared (ESO facilities) and gamma-ray (Fermi) observations. Other X-ray facilities will also be considered. We require 45 ks pointings taken every second revolution in order to 1) probe the physics of accretion by studying the 0.5--500 keV emission of the source 2) study the origin of the high variability of GRS 1915+105 3) understand the connections between accretion and ejection processes and 4) constrain physical models of emission processes. Points 1) and 2) can be done by looking into the interplay between the soft and hard X-ray emitters (therefore with JEM-X and IBIS) point 3) and 4) needs contemporaneous braod band coverages and timing studies. Besides these specific points this monitoring will allow us to accumulate more data and thus have a better view of the (rather unknown) behaviour of this source beyond 200 keV.  It should be noted that GRS 1915+105 lies in a quite crowded field with many variable sources such as X-ray binaries of all types the enigmatic microquasar SS 433 and a couple of highly absorbed IGR sources. This survey will also  permit all these sources to be studied in a regular manner. Such a monitoring will greatly participate to the INTEGRAL legacy by bringing new data on a dozen of exciting Galactic sources. [truncated! Please see actual data for full text]
DOI: 10.57780/esa-13wv2zv
title: 8860060

description: Crab  5x5 centered on-axis  2 degrees spacing
DOI: 10.57780/esa-14c9x5e
title: 1870002

description: In X-ray binary systems either a neutron star or a black hole accretes matter from an orbiting companion star. This accretion process often powers the launch of powerful relativistic collimated outflows called jets. While this connection between inflow and outflow is observed in systems ranging from forming stars to AGN jet formation remains poorly understood. Neutron stars in X-ray binaries offer a unique avenue to understand this process: as accreted material accumulates on the neutron star surface it can cause bursts of X-ray emission through runaway thermonuclear burning. The thermonuclear bursts can cool the surrounding structures such as the base of the jet. While these effects have been predicted from simulations such a response of the jet to thermonuclear bursts has never been observed directly.Our team have scheduled Australia Telescope Compact Array (ATCA) radio observations of an accreting neutron star to search for a response of the jet (brightness and morphology) to thermonuclear bursts. We have arranged with the INTEGRAL team to set up a simultaneous X-ray observation in order to measure when thermonuclear bursts occur for which we put in this official ToO. Comparing the INTEGRAL burst times with the radio light curve we will be able to test whether the jet responds by for instance briefly decreasing in power or by changing its spectrum. It will also reveal possible time delays between the X-ray and radio band probing the physical structure and size scales of the jet. The ATCA observations are planned for April 3 4 and 5 overlapping exactly with revolution 2350 of INTEGRAL. On April 3 they start at 12.30 GMT allowing for calibration before the start of the INTEGRAL revolution (at 13.18 GMT). The selected target is 4U 1728-34.  [truncated! Please see actual data for full text]
DOI: 10.57780/esa-14xx0mw
title: 1020018

description: Thermonuclear bursts in systems accreting pure helium reveal the structure of the neutron star (NS) interiors. In the absence of heating from steady H-burning between bursts the burst recurrence times and energetics are much more sensitive to the thermal properties and processes in the NS crust and core. Interestingly burst ignition models predict significantly longer burst recurrence times than observed for such sources. One way to resolve this discrepancy is fractional covering of the accreted fuel on the NS surface and recent analysis of a large sample of bursts from 4U 172834 appears to lend support to this hypothesis. However a large variation in the properties of bursts observed at similar accretion rates suggests that other processes perhaps including steady He-burning or incomplete burning may also be important.We propose to observe 4U 172834 with INTEGRAL and XMM-Newton simultaneously in order to measure the burst recurrence time and the persistent X-ray flux (and hence the accretion rate) in the broadest possible band to distinguish between these possibilities. The precise accretion rate measured over a wide multi-instrument energy band is crucial as it will enable detection of additional soft (or hard) spectral components outside the sensitivity band of individual detectors. The results of this study will provide stringent constraints for modeling of burst ignition conditions. [truncated! Please see actual data for full text]
DOI: 10.57780/esa-15i18p8
title: 0520035

description: We  ask  for up  to  3 INTEGRAL TOO observations of one blazar in outburst for a total of 600 ks  conditional to stringent  triggering  criteria  based on X-ray or  gamma-ray brightening as detected by the current high energy missions including INTEGRAL itself Swift/BAT and GLAST.  Coordinated  INTEGRAL and multiwavelength observations  will guarantee the coverage of a broad energy range and allow  us to follow the evolution of the overall  spectral  energy  distribution during one or more flaring episodes.  We will thus constrain  the  time-dependent  parameters of  the emission models.  In particular we would like to test in detail the scenarioin which for a given bolometric energy injected into a jet at different epochs large flux variations are observed  in individual frequency ranges depending on the size of the dissipation region. [truncated! Please see actual data for full text]
DOI: 10.57780/esa-184zrcc
title: 8860066

description: OMC FF sequence ISOC V10 onwards: sequence of ff measurements with LED on/off followed by a DC cal.
DOI: 10.57780/esa-18d9tvs
title: 8860235

description: OMC FF sequence ISOC V10 onwards: sequence of ff measurements with LED on/off followed by a DC cal.
DOI: 10.57780/esa-19gin0r
title: 0370002

description: INTEGRAL ToO on 4U 0142+61We request an INTEGRAL ToO on Anomalous X-ray Pulsar (AXP) 4U 0142+61 now that it is in an extended active state with bursting activity observed in RXTE monitoring data (Dib et al 2006 Atel 845). It is essential to observe this AXP soon preferably within a week to study the hard X-ray spectrum with JEM-X and ISGRI.  [truncated! Please see actual data for full text]
DOI: 10.57780/esa-1afeomy
title: 1470008

description: 4U 1543-624 is an X-ray binary likely harboring a neutron star in an18-minute binary orbit. Though it is a persistent source theSwift/BAT now shows a clear rising flux trend in 15-40 keV  the source has never shown behavior like this in the past. This differs somewhat from other persistent sources such as Z and Atoll sources that vary in quasi-regular patterns. It also differs from the behavior observed in true transient sources with short periods such as SAX J1808.4-3658. The outburst behavior may represent a change in the corona of this source and a study of coronal evolution in an UCXB is relatively unexplored territory.  [truncated! Please see actual data for full text]
DOI: 10.57780/esa-1cdw6qd
title: 1570011

description: Coordinated observation of 3C 273
DOI: 10.57780/esa-1dt86is
title: 0720027

description: On Jan. 22 2009 a huge outburst of 1E1547.0-5408 commenced accompanied by strongly increased short-duration burst activity. INTEGRAL detected emission up to ~150 keV during 2 ToO observations one performed for about 100 ks on Jan. 24-25 2009 and a second for 600 ks from Jan. 28 to Feb. 8 2009.Till this outburst no INTEGRAL detection could be established. Now for the first time INTEGRAL discovered the turn-on of hard (photon index ~ 1.3  pulsed) emission. During the second INTEGRAL ToO the source was still (very) bright between 20 and 150 keV with no signs of fading. Its flux decreased only 30% compared to the first ToO measurement. The biggest question therefore is whether this hard tail will fade or will remain stable like the persistent hard X-ray emission from the other three AXPs showing hard spectral tails?  Therefore we propose to reobserve 1E1547.0-5408 for 2 revolutions (~400 ks) during AO7. [truncated! Please see actual data for full text]
DOI: 10.57780/esa-1empyat
title: 0120016

description: The soft gamma repeaters (SGRs) are suspected to be magnetars objects in which the magnetic field energy dominates all other energy sources including rotation.  SGRs go through phases of intense activity during which they may emit hundreds of bursts within a period of weeks or so.  During those periods they exhibit properties which are quite different from their quiescent properties.  Their strong magnetic fields are probably responsible for these changes and accordingly it is interesting to study them intensely at these times.  We propose two ToO observations of any of the known or of any newly discovered SGRs during their active phases.  For clarity we have filled out one observation form for each of the known SGRs and for one unknown SGR.  Our total request however is for justTWO ToOs. [truncated! Please see actual data for full text]
DOI: 10.57780/esa-1glxae2
title: 0720003

description: Recently significant advances have been made in  understanding of the diffuse Galactic continuum emission observed by SPI on INTEGRAL. The hard power-law component has been identified with inverse-Compton emission from relativistic (GeV) electrons on the cosmic microwave background and Galactic infrared radiation field. The observed intensity is in good agreement with detailed predictions from the GALPROP model which accounts for both primary and secondary electrons and positrons.  We propose to exploit this with INTEGRAL to obtain a probe of the distribution of cosmic-ray electrons in the Galaxy in particular in the Galactic halo seen at high latitudes. To this end we propose a multi-year scan covering a wide latitude range in the inner Galaxy significantly deepening the exposure over what is currently available. The decreasing background due to the solar cycle will improve the signal-to-noise over that for the INTEGRAL   mission so far.The results will have implications for Fermi-LAT which will be in operation during this period - taken togetherthe data from the  two missions will constrain the cosmic-ray electron spectrum at GeV energies and help to give an unambiguous decomposition of the diffuse gamma-ray sky. [truncated! Please see actual data for full text]
DOI: 10.57780/esa-1k4s3pj
title: 1570005

description: The X-ray burster IGR J17379-3747 was discovered by INTEGRAL in 2006 during the search for X-ray type-I burst in INTEGRAL archive (Chelovekov and Grebenev 2006). The burst recorded on February 2004 by the IBIS/ISGRI telescope could not be identified with any of the then known persistent X-ray sources. On September 2008 the source was observed in outburst again by INTEGRAL and Swift (Atel #1711 #1714) with an X-ray localisation of: RA (J2000): 17h 37m 58.81sDec (J2000): -37d 46m 19.6s with an uncertainty of 1.4 (90% confidence). The presence of type-I bursts revealed the low-mass X-ray binary (LMXB) nature of the system in which the compact object is likely a weakly-magnetised neutron star.On 2018 March 19 MAXI/GSC reported renewed X-ray activity from IGR J17379-3747 (Atel #11447) that was confirmed on March 23 by Swift/XRT that localised the source at position consistent with errors with the known position of the source.An XMM ToO has been granted to our group (PI: A. Sanna). We request here a possible simultaneous observation with INTEGRAL to perform a broad-band spectral analysis. [truncated! Please see actual data for full text]
DOI: 10.57780/esa-1kges4a
title: 0120148

description: SN1987 A in the Large Magellanic Cloud is a once-in-a-lifetime opportunity to observe gamma-ray emission from a Type II supernova with INTEGRAL. The radioactive isotope 44Ti emitter of gamma-ray photons at 67.9 78.4 and 1157 keV is an ideal tracer to probe core collapse physics since it is created in appreciable amounts in the innermost layers of the exploding star. Radioactive decay of 60Co accompanied by gamma-ray line emission at 1173 and 1332 keV is sensitive to the neutron excess in the supernova providing a unique chance for a direct measurement of this important parameter. Therefore we propose to search for the gamma-ray line signatures that arise from the decay of 44Ti and 60Co produced in SN1987 A. The measurement of the gamma-ray line fluxes will allow the determination of the 44Ti and 60Co yields in SN1987 A providing information about the position of the mass-cut the maximum temperature and density reached during the passage of the shock wave in the ejecta and the neutron excess. The 44Ti line profile will provide excellent information about the velocity structure of the ejecta close to the mass-cut and probes the pre-supernova composition inside 2 Msol. We will use both SPI and IBIS to search for the three gamma-ray lines of 44Ti although we only expect to detect the 1157 keV line with SPI within the requested 2000 kiloseconds of exposure time. 60Co is certainly an observational challenge but due to the rapid decay of this isotope INTEGRAL probably represents the last chance to measure its gamma-ray lines in SN1987 A. In addition to the 2000 kiloseconds we also request the data rights for all additional observations of the LMC region in order to search for the 44Ti and 60Co decay signatures of SN1987 A. [truncated! Please see actual data for full text]
DOI: 10.57780/esa-1kqwkjd
title: 0199921

description: Galactic Centre Deep Exposure for cycle 2 pattern 1
DOI: 10.57780/esa-1md6prw
title: 0520068

description: We propose to monitor the evolution of the cyclotron lines in the Be transient 4U0115+63 throughout its next  major outburst which is expected to happen in 2008. The aim of our observations is to study the luminosity dependent evolution of the cyclotron line which is probably due to changes in the height of  the accretion column caused by the varying mass accretion rate over the outburst.  [truncated! Please see actual data for full text]
DOI: 10.57780/esa-1oc3by9
title: 8860301

description: SAS Calibration in Rev 1405
DOI: 10.57780/esa-1ortxka
title: 0120236

description: A hard X-ray component extending up to several hundred keV has been recently discovered in Sco X-1 and a few others Z-sources i.e. low mass X-ray binaries LMXRBs which host an old weakly magnetized and fastly spinning neutron star accreting at rates close to the Eddington limit. Among sources accreting at near-Eddington rates only black hole candidates (BHC) were known to possess similar high energy tails. A variety of models for the hard X-ray components of BHCs has been proposed including thermal non thermal and bulk motion COmptonisation shock emission or annihilation in a pair dominated plasma cloud. The presence of a similar hard component in Z-sources opens up a new area of investigation for neutron stars accreting at high rates. Z-sources are known to have highly variable radio counterparts indicating episodic ejection of matter at relativistic energies. Recent observations of the radio source associated with Sco X-1 revealed variable lobes on opposite sidesof the central source propagating outwards at about 0.4-0.5 c. A detailed investigation of these phenomena in Sco X-1 and the extent to which they parallel those observed in stellar mass BHCs is the main aim of our program. This is based on coordinated observations to be carried out simultaneously from soft gamma ray to X-ray energies and in the V-band near-IR and radio. We request a sigle 300 ksec INTEGRAL observation. In particular we will:(a) study the correlated variability from the soft gamma rays to the radio (b) investigate the hard X-ray continuum of the source up to energies of ~ 700-800 keV and its relation to the source state as determined through multiwavelength observations (c) search for high energy emission lines similar to those observed in Nova Muscae 1991. [truncated! Please see actual data for full text]
DOI: 10.57780/esa-1ptk7af
title: 0299835

description: Galactic Plane Survey for AO 02 and Pattern 35
DOI: 10.57780/esa-1qm6q83
title: 8860200

description: OMC FF sequence ISOC V10 onwards: sequence of ff measurements with LED on/off followed by a DC cal.
DOI: 10.57780/esa-1rdlgk5
title: 0299913

description: Galactic Centre Deep Exposure for AO 02 and Pattern 13
DOI: 10.57780/esa-1t2u85h
title: 1520023

description: One of the most important results on Galactic black holes that has come out of INTEGRAL was the discovery of the signature of strong polarization of the >300 keV spectrum of Cygnus X-1. This discovery is an indication that this spectral component is due to synchrotron emission probably from the radio jet that is present in the hard state. In this two year 2 Ms program we propose a continuation of these measurements with the aim of detecting changes in the hard state polarization properties. [truncated! Please see actual data for full text]
DOI: 10.57780/esa-1t8uz58
title: 0420083

description: We propose to study the pre-periastron flare of GX 301-2 by observingfour pre-periastron flares resulting in a total observation time of600 ksec. This will allow us to study the structure (includingdensity and clumpiness) of the gas stream flowing from Wray 977 to GX 301-2which is intercepted by the neutron star prior to periastron passagegiving rise to the pre-periastron flare. As the source is verybright during the flare spectra with high statistical quality up to100 keV will be obtained. These will then be used for phaseresolved spectroscopy to study the spectral variation (esp. thecyclotron line) with pulse phase and to search for a harmonicline. The obtained flare data will be complemented by substantialarchival data taken outside the flare for comparison. Such a studyis not possible with archival data as there is almost no coverage of the pre-periastron flare. [truncated! Please see actual data for full text]
DOI: 10.57780/esa-1vl4gk0
title: 1140002

description: We ask for INTEGRAL TOO observations of one blazar in outburst in AO-11 for up to 600 ks conditional to stringent triggering criteria based on X-ray  brightening as detected by the current high energy missions including INTEGRAL itself Swift MAXI and NuSTAR. Coordinated INTEGRAL and  multiwavelength observations will guarantee the coverage of a broad energy range and allow us to follow the evolution of the overall spectral energy distribution (SED) during one or more flaring episodes. We will thus measure accurately the high energy spectrum and monitor the hard X-ray light curve  and thus constrain the time-dependent parameters of the emission models. In past INTEGRAL AOs we have triggered similar observations as part of multi wavelength campaigns and have demonstrated that for bright X-ray sources (> 20 mCrab in 2-10 keV) IBIS can map the interday hard X-ray variability. [truncated! Please see actual data for full text]
DOI: 10.57780/esa-1wmktwd
title: 1520025

description: This proposal is aimed on obtaining legacy-level observational datasets on the Milky Way Galactic disk.  The ultimate goal of the entire project is to have model independent and systematics free measurements of the fluxes in nuclear lines (511 keV annihilation emission and 1.8 MeV Al26) and a broad band spectrum of the Galactic background emission which at different energies is provided either by cumulative emission of faint Galactic source or by interaction of low energy cosmic rays with interstellar medium. Taking into account the unique combination of properties of INTEGRAL instruments - broad band coverage large fields of view and possibilities to eliminate the contribution of discrete sources from the total measured photon flux the proposed strategy is the best possible usage of the valuable INTEGRAL time. Wide mapping of the Milky Way during the campaign of Galactic latitude scans also contributes to the legacy of the INTEGRAL observatory giving the opportunity to study the population of Galactic sources at high latitudes. [truncated! Please see actual data for full text]
DOI: 10.57780/esa-1ws8qs6
title: 0270002

description: TOO observation of 3C 273 in low mm stateWe want to observe 3C 273 in revolution 207
DOI: 10.57780/esa-1y1fguw
title: 0120102

description: We propose 4 observations (75 ks each) of Cygnus X-1 in the hard state.For each individual observation the broadband coverage of INTEGRAL will enable us to study for the first time the spectral and timing characteristics of the emission above 200 keV together with the lower energy and down to 3 keV.In particular thanks to the timing capabilities of INTEGRAL we will learn the characteristics the rapid aperiodic variability above 200 keV (power spectra time-lags with othe renergy bands...).We will perform simultaneous radio IR and optical observations and search for timing correlations between these wavelengths and the high energy emission. We will focus on the expected (but not detected yet)  timing  correlations on short time-scales (minutes hours).The comparisons between the different observations will allow the first comprehensive study of the broad-band spectral evolution:  in particular we will search for correlated  changes in the spectral parameters (spectral slopereflection amplitude cut-off energy and shape) on time-scales > 2 days. The multi-wavelength coverage will reveal how the radio/IR/optical spectrum changes (or not)  when the high energy spectrum change. The long term fluctuations of the timing properties will be studied in parallel to the spectral evolutions with the aim of searching for spectro/timing correlations. These observations will address the following points:what is the nature of the emitting plasma e+-e- or e--p? What is the geometry of the inner accretion flow  (central spherical hot corona surrounded by a cold disk or a patchy corona atop the a cold disc)? How does the ejection process take place and in particular what is the nature of the link between the Comptonising corona and the jet ?What is the nature of the excess above 200 keV (non-thermal processes multi-temperature Comptonisation...) ? What is the mechanism of short term variability ? [truncated! Please see actual data for full text]
DOI: 10.57780/esa-20kzuap
title: 1970008

description: End to end test of Fast TOO procedure
DOI: 10.57780/esa-219vu9p
title: 1770004

description: INTEGRAL TOO observations of the Crab in coordination with ART-XC onboard Spekt-RG
DOI: 10.57780/esa-236wezf
title: 0399809

description: Galactic Plane Survey for AO 03 and Pattern 09
DOI: 10.57780/esa-25p5033
title: 8860283

description: Crab observations during 1281
DOI: 10.57780/esa-2883hbz
title: 1720025

description: We propose a multi-year program of ultra-deep observations of the M81 extragalactic field. This survey will constitute INTEGRAL legacy for the study of the AGN population at low hard X-ray fluxes and provide unique synergy with the upcoming all-sky survey by the eROSITA and ART-XC telescopes onboard the Spectrum-Roentgen-Gamma spacecraft. We ask for 5 Ms observations to be performed in the standard 5x5 dithering pattern during 2019-2020. We are planning to ask for an additional 5 Ms after completion of this proposal. [truncated! Please see actual data for full text]
DOI: 10.57780/esa-29eik25
title: 8860043

description: OMC FF sequence.Contains a sequence of 5 FF observations followed by short observation with OMC in standbyfollowed by DC calibration observationfollowed by short observation with OMC in standbyobservation scheduling constraints: at least 10h after perigee and not under Goldstone coverage [truncated! Please see actual data for full text]