cometadata/datacite-titles-descriptions-related-identifiers huggingface dataset:
DOI: 10.57780/esa-elokpcf
title: 1020029

description: We propose an additional deep 3.0 Msec exposure of the Large Magellanic Cloud in order 1). to confidently detect and precisely measure the flux from SN 1987A in the direct-escape lines of radioactive Ti-44 (lines at 67.9 78.4 and 511 keV) 2). to study possible hard X-ray emission produced by cosmic-rays accelerated in the ejecta blast wave interacting with the ``inner equatorial ring of circumstellar material of SNR 1987A 3) to search for hard emission from the stellar remnant of this supernova (or significantly improve the existing upper limit). This proposal is a continuation of our proposals approved by TAC in AO-7 (for observations with a 2.0 Msec exposure) and AO-8 (for observations with a 1.5 Msec exposure). If the additional 3.0 Msec observations of the region will be carried out in AO-9 the total exposure for SN1987A will be increased till 9 Msec - by a factor of 2 relatively the presently available one - that will allow INTEGRAL to confidently detect the Ti-44 radioactive lines. In addition to the above (main) purposes of the proposals we will try to detect an electron-positron annihilation line from the dark bulge of the LMC (testing the hypothesis that the line can be produced in the LMC and in the Galactic center by dark matter annihilation). The deep observation of the LMC will also allow ones to monitor X-ray variability of a number of compact X-ray sources present in the field and search for new X-ray transients and weak sources. This observation makes the best use of the unique INTEGRAL capabilities and undoubtedly is the most efficient investment of its precious observing time. [truncated! Please see actual data for full text]
DOI: 10.57780/esa-en3jmwl
title: 1220022

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 1.8 MeV Al26 and 1.17 MeV and 1.33 MeV Fe60 lines) 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-enllail
title: 1320019

description: Diffuse line emission from radioactive 26Al has been observed throughout the Galaxy and is one of the key science goals and assets of the INTEGRAL mission. INTEGRAL has provided a new image of the Galaxy in 26Al gamma-rays and has provided high-resolution spectra as a new astronomical measurement. This has led to a multi-wavelength test of massive-star nucleosynthesis for groups of stars comparing the INTEGRAL measurement to the richness of massive star clusters and their effects on surroundings other than the radioactive nucleosynthesis ejecta which are ionization of surrounding gas and cavities created in the ambient interstellar medium. Much has been learned from the brightest such nearby massive-star groups. Also on the Galactic scale the measured Doppler shifts from large scale Galactic rotation have led to a proposition of massive-star ejecta recycling preferentially through large superbubbles located between spiral arms. This was derived from the discrepancy of 26Al gas velocities to other objects participating in Galactic large-scale rotation.  60Fe radioactivity is assumed to arise from the same massive star groups except that it only is ejected from the later core collapse explosions rather than from Wolf-Rayet phase winds and supernovae as 26Al is. The ratio of 26Al to 60Fe emission for groups of stars provides us with a test of the models for massive-star interiors.Here we request data rights for all observations that cover different regions throughout the Galaxy with respect to analysis for 26Al emission and also for the fainter emission in 60Fe gamma-rays that is expected to correlate with 26Al. Additionally we propose that if the exposure of the disk is to be made more homogeneous the Carina region would be a suitable place to do so. [truncated! Please see actual data for full text]
DOI: 10.57780/esa-eomcxt6
title: 0299831

description: Galactic Plane Survey for AO 02 and Pattern 31
DOI: 10.57780/esa-epyxoox
title: 0120212

description: This is a proposal to carry out the first hard X-ray/gamma-ray study of the Small Magellanic Cloud. The combined timing and imaging ability of INTEGRAL will permit a detailed study of the surprisingly large population of High Mass X-ray Binaries in this galaxy. It will provide the first opportunity to study a whole class of objects in a different environment from our Milky Way and to address some fundamental questions related to the evolution of these systems and their exceptionally large luminosity variations.  We also expect that from these observations we will be able to deduce some vital clues into the star formation history of the SMC. [truncated! Please see actual data for full text]
DOI: 10.57780/esa-eqptnkf
title: 8860209

description: This is a dummy pointing!
DOI: 10.57780/esa-erh81b7
title: 0299823

description: Galactic Plane Survey for AO 02 and Pattern 23
DOI: 10.57780/esa-ertvtsl
title: 0510001

description: AO-5 CP: Deep obs. of Galactic Plane.Improve uniformity of exposure in Galactic plane.
DOI: 10.57780/esa-es353om
title: 1420001

description: The Galactic bulge region is a rich host of variable X-ray and gamma-ray point sources. Since AO-3 we are monitoring about 190 of them with one hexagonal pattern about every 3 days whenever the region is visible by INTEGRAL. Due to the high scientific return and in order to preserve the continuity with respect to past observations of this ever-changing region we propose to continue our successful program. Our main aim is to monitor and actively report on any (transient) activity  in the long run the program is providing regular and homogeneous inputs about the soft and hard-X-ray (transient) population as well as on the accretion regimes in the various types of binary systems. As a service to the scientific community the observations are to be made public. We will continue to make the IBIS/ISGRI and JEM-X quick-look results publicly available through the web soon after the data have been taken to preserve the possibility for rapid follow-up by the community. [truncated! Please see actual data for full text]
DOI: 10.57780/esa-esojr07
title: 1570003

description: Black hole transients (BHT) are the only class of black holes (BH) which samples a wide range of accretion rates and accretion states during their month to year long outbursts. BHT classically show two types of outflows: collimated radio-jets ubiquitous during the canonical hard state and highly ionised X-ray winds during the soft state. We propose a combined XMM+NuSTAR monitoring campaign of an high inclination BHT to shed light on the evolution of the wind while the source transits through the intermediate states.  [truncated! Please see actual data for full text]
DOI: 10.57780/esa-eubs0fm
title: 1020003

description: For the first 5 years of INTEGRALs operational life the scientific Core Programme included a keycomponent that was regular scans of the Galactic Plane. These led to a wealth of discoveries of new sources and source types a large fraction of which were highly transient. These discoveries can certainly be considered one of the strongest results from and legacies of INTEGRAL. From AO-5 onwards these regular scans were discontinued and this resulted in a significant drop in the discovery rate of new systems in and around the plane of our Galaxy. In AO8 however a multiyear proposal to reinstate the scans was approved and the programme is still on going in AO9. We propose here to continue the Galactic Plane Scans as a Key Programme throughout AO10 and AO11 to regularly monitor known systems as well as to dramatically enhance the chances of discovering new systems. This will allow a rapid response to bright events and a detailed study of faint transients and long term activity. Such a programme will be of high value to a very large fraction of the high-energy astronomy community stimulating science immediately and furthermore contributing greatly to the INTEGRAL legacy.To this aim a total of 3 Msec (1 in AO101 and 2 in AO11) of observations is necessary to cover theplane with regular scans every orbit excluding the central zone that will be covered by the GalacticBulge monitoring programme (should that programme be accepted) and any other region studieddeeply in other proposals. We suggest that in order to maximise the engagement of the scientificcommunity the observations should be made public immediately. The team will make as it is alreadydoing through AO8-9 the scw-resolution IBIS and JEM-X light curves (in two energy bands) and perrevolution mosaic images publicly available through the web as soon as possible.  Any interesting source behaviour that emerges from our observations will be announced prompt [truncated! Please see actual data for full text]
DOI: 10.57780/esa-eywaixj
title: 0120207

description: We aim to investigate on a wider energy band the spectral behaviour of two already detected reported hard X-ray bursters to better determine the spectral parameters (presence of an energy cut-off reflection component etc.) study the accretion flow around the compact object and hence to firmly establish the still unclear emission origin. This as a part of long term programme started with BeppoSAX.The BeppoSAX and RossiXTE telescopes allowed for the first time to perform simultaneous high energy observations of classes of objects on a wide energy band. A high energy component in the spectra of X-Ray bursters firstly discovered by SIGMA has been detected with the NFIs (Narrow Field Instruments) on board BeppoSAX from at least 15 sources confirmning these objects as hard X-ray emitters. Similarity of Black Hole and Neutron Star spectra as well as variability when in Low State suggest the same mechanism to power the hard X-ray emission. Still controversial remain observational criteria to distinguish these two types of accreting systems apart from clear timing signature such as X-ray pulsation or X-ray bursts.We require total of 2 x 300 ksec to be spent on 2 bursters whose hard X-ray properties need for key investigation at high energy to disentangle their soft gamma ray emission processes: X1916-053 and X2127+119. [truncated! Please see actual data for full text]
DOI: 10.57780/esa-ezo7qdw
title: 8860309

description: OMC FF sequence ISOC V10 onwards: sequence of ff measurements with LED on/off followed by a DC cal.
DOI: 10.57780/esa-f1n8e00
title: 0520018

description: GRS 1915 is a key target for the understanding of microquasars and accreting black holes in general. It can undergo on short timescales (sec-min) transitions that occur on longer timescales (~days to weeks) in other sources. We hence can catch them very easily while pointing INTEGRAL and thus have an unique chance to understand their physical origin through a broad band (spectral and temporal) study of the source. We then propose to continue the monitoring of  GRS 1915+105 and its surroundings during AO5. 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 Nancay) and infrared (ESO) observations.  IBIS JEM-X are  the prime instruments for this study together with SPI in cases of steady states. 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 attention to 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 p [truncated! Please see actual data for full text]
DOI: 10.57780/esa-f2wb44h
title: 0399807

description: Galactic Plane Survey for AO 03 and Pattern 07
DOI: 10.57780/esa-f3c54iq
title: 1820008

description: The survey of the Galactic Plane has continued as one of the main INTEGRAL scientific objectives because of the scientific potential of both new source discovery and detailed monitoring of already known sources that will provide a legacy archive and a basis for future missions. We propose for a total of 3.0 Ms of observations in AO18 and 3 Ms in AO19 to continue our KeyProgram covering areas of the Plane with regular scans every orbit. For these AOs we selected again the section of the Plane incorporating two sky regions centered at l=+/-30 that are both rich in galactic sources (LMXB and HMXB SFXT inparticular) and potential MeV/TeV sources. Our purpose is to regularly monitor known systems as well as to dramatically enhance the chances of discovering new systems or new outbursts from known sources. This program will allow a rapid response to bright events and a detailed study of faint transients and their long-term activity. Such a programme will be of high value to avery large fraction of the high-energy astronomy community stimulating science immediately and furthermore contributing greatly to the INTEGRAL legacy. In order to maximise the engagement of the scientific community we will continue to make the observations public immediately. The team will make as it has been through AO8-17 the scw-resolution IBIS and JEM-X light curves (in two energy bands) and per revolution mosaic images publicly available through the web as soon as possible. Any interesting source behaviour that emerges from our observations will be announced promptly in the usual way through Atels so that rapid follow-up by the community is possible as has already been demonstrated. [truncated! Please see actual data for full text]
DOI: 10.57780/esa-f3d5hdc
title: 8860201

description: OMC FF sequence ISOC V10 onwards: sequence of ff measurements with LED on/off followed by a DC cal.
DOI: 10.57780/esa-f40xmnj
title: 1870007

description: INTEGRAL TOO observations of  V4641 Sgr
DOI: 10.57780/esa-f4dikkn
title: 8860260

description: Crab 2012: SPI/IBIS 5x5 wide rev 1214
DOI: 10.57780/esa-f93h32t
title: 1270001

description: SAX J1748.8-2021  is most probably an accreting millisecond pulsar according to the spectral shape and location in the sky. INTEGRAL observations would be the only mean of studying its pulsations because Swift has not the timing resolution to achieve this scope.Since it is ill an interesting source and worthwhile to spent time upon a public out-of-TAC TOO proposal was accepted with a 100 ksec observation to be done in revolution 1511 (starting monday Feb 23).  [truncated! Please see actual data for full text]
DOI: 10.57780/esa-f969vld
title: 1720013

description: One of the most important results on Galactic black holes that has come out of INTEGRALwas 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 probablyfrom the radio jet that is present in the hard state. In this two year 2 Ms program we propose acontinuation of these measurements with the aim of detecting changes in the hard state polarizationproperties to set strong limits on the hard tail in the soft state and to break degeneracies between thetwo families of models for the formation of the hard tail. [truncated! Please see actual data for full text]
DOI: 10.57780/esa-f9fga0n
title: 0720049

description: This proposal is a one of three accompanying proposals aimed on obtaining legacy-level observational datasets on the Milky Way Galactic disk. The ultimate goal of the entire project (which started in AO4 and which we plan to continue it in subsequent AOs) is to have model  independent and systematics free measurements of the fluxes in nuclear lines (511 keV annihilation emission 1.8 MeV 26Al and 1.17 MeV and 1.33 MeV 60Fe lines) 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. Our strategy was supported by INTEGRAL TACs during previous AOs and now we propose to continue the coverage of the Galactic disk with scanning observations.  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 descrete sources from the total measured photon flux the proposed strategy is the best possible usage of the valuable INTEGRAL time.In this proposal we ask for 1.5 Msec observations of outer galactic region at l=155 deg which will be complimentary to the already performed observations of the inner Galaxy at l~40 22.5 and -45 deg. This is one of the two underexposed regions of the Galaxy. Here we were driven largely by the INTEGRAL Legasy consideration. It is important that the whole galactic plane is mapped with INTEGRAL. With these observations we will continue the mapping of the GRXE namely put upper limits to hard X-ray emission generating by accreting White Dwarfs in the Galaxy. It is possible that gamma-ray continuum emission of the Galactic diskwill not be detected at such large distances from the Galactic Center however any measurement of the Galactic emission  will be useful for constraining the models of the cosmic ray induce [truncated! Please see actual data for full text]
DOI: 10.57780/esa-f9xxsmp
title: 0299820

description: Galactic Plane Survey for AO 02 and Pattern 20
DOI: 10.57780/esa-fakzvua
title: 1220043

description: The Large  and  Small Magellanic Clouds (LMC  and  SMC) represent an exceptional opportunity to study the evolution of X-ray binaries (XRB) under very different conditions to those in the Milky Way. The Clouds are close enough for the individual sources to be detected identified  and  studied whilst presenting diverse environments in terms of metallicity and tidal effects. In addition the population as a whole is possibly greater than the comparable Milky Way population so it provides an invaluable test-bed for accretion physics  and  binary evolution. This programme will carry out regular monitoring of the SMC to locate new transient pulsar systems and to continue exploring the ~100 known  and  suspected HMXB systems.  [truncated! Please see actual data for full text]
DOI: 10.57780/esa-fbck8ql
title: 1920018

description: Despite decades of observations the nature of the hard X-ray/soft gamma-ray emission of Cen A the brightestradio-loud AGN in the hard X-ray sky is still unclear. The two main competing models are thermal Comptonizationand synchrotron self-Compton emission and they predicted a spectral cutoff of roughly 300 keV or above 1 MeVrespectively and requires spectral coverage out to the MeV region to differentiate. INTEGRAL/SPI has spectral coverageto a few MeV and thus capability to constrain where the spectral cutoff occurs and assess the origin of the hardX-ray/soft gamma-ray emission. SPIs high energy resolution can also search for 511 keV annihilation features inthe spectrum on both short and long timescales. Motivated by this we request a multi-year normal time proposal of3 Ms of exposure time in AO-19 and 3 Ms on exposure time in AO-20. [truncated! Please see actual data for full text]
DOI: 10.57780/esa-fbfp4d8
title: 0299914

description: Galactic Centre Deep Exposure for AO 02 and Pattern 14
DOI: 10.57780/esa-fblgpnx
title: 2070002

description: INTEGRAL TOO Observations of RXS J044100.3
DOI: 10.57780/esa-fd34io7
title: 8860012

description: Calibration observation 3 - 2nd part: 135 ksec observation 7.4 degree offset from Cygnus X-1. Observation executed after formal end of Commissioningphase. This completes the 270ksec required  to study the PSF extended and diffuse emissionline emission imaging capabilities in crowded fields crosscalibratoin and demonstration of IBIS imagingcapability in dither mode. In addition is this observation suitable to study the background evolution. [truncated! Please see actual data for full text]
DOI: 10.57780/esa-fdu5mrr
title: 1470011

description:  PSR J2032+4127/ MT91 213 was identified as a pulsar/Be-star binary through radio and gamma-ray timing observations (Lyne et al. MNRAS 451 581 2015  Ho et al. MNRAS 464 1211H 2017). It has recently enhanced flux across the spectrum from Optical to TeV gamma-ray that are apparently associated with the upcoming periastron passage. The orbit of of PSR J2032+4127/ MT91 213 is highly eccentric (45 yrs < p < 50 yrs and 0.96 < e < 0.99) and is expected to reach periastron sometime around November 2017. Enhanced activity is expected before and after the periastron passage and flaring events are also expected as the pulsar moves through the stellar disk. This system is near in the sky to unknown gamma-ray source TeV J2032+4130 which is thought to be the pulsar wind nebulae (PWN) counterpart of PSR J2032+4127 (Aliu et al. ApJ 783 16 2014). This rare event may help to determine if the TeV source is associated with a component in this binary system.Recent TeV gamma-ray observations from VERITAS and MAGIC have been summarized in an Astronomers Telegram on October 2 2017 (http://www.astronomerstelegram.org  ATel #10810). The recent optical/UV/x-ray observations from Swift-XRT Swift-UVOT and 2m Liverpool Telescope are summarized in an Astronomers Telegram on October 15 2017 (ATel #10851). Observations taken prior to July 2017 by VERITAS did not detect the binary system and the x-ray flux detected by Swift-XRT has been slowly increasing over the past year (Bird et al. arXiv:1708.04718 and Li et al. ApJ 843 85L 2017). More recent observations in September 2017 by VERITAS show that the flux measured in TeV gamma-rays has doubled to 4.2e-12 photons/cm2/s (above 200 GeV) resulting in a significant detection at the location of the pulsar and is expected to increase further. More recent observations from Swift-XRT in October 2017 show that the x-ray flux (0.3-10keV) has increased at least 5 times average fl [truncated! Please see actual data for full text]
DOI: 10.57780/esa-fjq1sxd
title: 8860165

description: Crab-2007 Spring: SPI 5x5 pattern