cometadata/datacite-titles-descriptions-related-identifiers huggingface dataset:
DOI: 10.57780/esa-l86zv6n
title: 0720026

description: We propose that the Cygnus region be considered as a key target of INTEGRAL in order to answer fundamental questions related to the nucleosynthesis of massive stars and the production and transport of galactic positrons. Our proposal follows the 2x2Ms that have been granted in the AO5 and AO6 cycle. We ask for 2Ms to be performed in AO7 and request a long-term observational effort to allow significant progresses on nucleosynthesis and annihilation. The Cygnus region is the most nearby massive star forming region in our Galaxy with about 200 O stars located at about 1.5kpc. This richness and proximity make it possible to get an accurate picture of the region and allow in the same time a clear detection of the 1809keV line of the 26Al synthesised by massive stars. The first years of INTEGRAL have allowed to attribute the most of this emission to the Cyg OB2 young cluster thereby confirming the contribution of stellar winds to the ejection of 26Al and validating the recent improvements of stellar models. With additional observing time we will be able to evaluate more accurately the morphology of the 1809keV emission and to relate it to specific stellar groups. Current theoretical estimates also show that we may be close to detect the 1173/1332keV emission from the decay of the 60Fe released by supernova explosions. These advances will be strong constraints on the stellar models. A substantial increase of the exposure on Cygnus will also lead to the detection of the 511keV annihilation signal and/or constrain the diffusion regime of the galactic positrons as well as the existence of disk positron sources other than 26Al. Both aspects are essential to the understanding of the 511keV galactic emission observed to come mostly from the galactic bulge. All these science prospects fully justify the substantial INTEGRAL observing time we require. In addition the Cygnus region is rich in compact objects thus ensuring the in [truncated! Please see actual data for full text]
DOI: 10.57780/esa-lcxfl93
title: 8860011

description: OMC flat field #8 to be executed at the end of PV (rev25). Full sequence where both readout nodes are used.Observation parameters according to JNs email from 05/Sep/2002.Note it is not required to enter the exact start time for each observation but it has to be ensured that thestart time of observations with a higher ID is later than the earlier ones. Observation 20 must  be executed as last observation to reconfigure OMC. [truncated! Please see actual data for full text]
DOI: 10.57780/esa-ld4ssrb
title: 8860291

description: OMC FF sequence ISOC V10 onwards: sequence of ff measurements with LED on/off followed by a DC cal.
DOI: 10.57780/esa-lg3f1i4
title: 1360001

description: Coordinated observations of 3C 273
DOI: 10.57780/esa-lhf03nc
title: 1420030

description: We propose to observe the repeating fast radio burst FRB 121102 using the Integral satellite and the Arecibo Effelsberg and Nancay radio telescopes in order to search for a high energy emission simultaneously with radio measurements and to look for a possible afterglow. Fast radio bursts (FRBs) are bright flashes of radio waves that last only a few thousandths of a second whose origin is currently unknown. Initially thought to come from a cataclysmic and unique event the recent detection of repeating bursts from FRB 121102 at a frequency of 3 bursts/hour indicate that they may originate from different types of progenitors. Giant flares from magnetars or giant radio pulses from pulsars are possible sources of the FRBs. In such detecting a high energy signal (burst and/or afterglow) from FRB 121102 will help to define the class of the object responsible of this huge energetic event and to better characterize the physics at work in such astronomical system. The timing capabilities of the X and gamma-rays instruments on board the Integral satellite (better that 100 microseconds for JEM-X IBIS and SPI - SPI/ACS with 50 msec time resolution not being r^ant at least for the burst detection -) combined with the exquisite timing resolution supplied by the Nancay Radio telescope and other major radio facilities in the world as Arecibo and Effelsberg will be even if presently submitted as an exploratory programme the first step to study in the high energy range this new and promising new class of astronomical objects. [truncated! Please see actual data for full text]
DOI: 10.57780/esa-lidva0e
title: 0720010

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 understand how the accretion onto the compact object proceeds. To help answer these questions 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 plus another 2 Msec in the next AO) a unique region of the sky where two of the brightest known ULXs are located: M82 X-1 and Holmberg IX X-1. We will measure the spectra of these sources from 3 keV up to 50-100 keV and study their spectral variability. We will also analyze the hard X-ray spectrum of the low-luminosity AGN M81 located in the same field. [truncated! Please see actual data for full text]
DOI: 10.57780/esa-lmgz4xx
title: 8860337

description: OMC FF sequence ISOC V10 onwards: sequence of ff measurements with LED on/off followed by a DC cal.
DOI: 10.57780/esa-lqpow6d
title: 8860380

description: Crab Calibration 2017.2 (1856-57): IBIS/SPI
DOI: 10.57780/esa-lqyhicm
title: 8860128

description: OMC FF sequence ISOC V10 onwards: sequence of ff measurements with LED on/off followed by a DC cal.
DOI: 10.57780/esa-lsl7ry6
title: 0720011

description: Over last years it was firmly established that luminous accreting  neutron stars demonstrate high energy tails in their spectra which while  is very minor in terms of energy budget of a source can tell us a lot about  physical processes occuring in the innermost regions of the accretion flow. In particular  one can anticipate appearance of the high energy tail due to presence of hot optically thin corona above optically thick main emitting regions of the flow which might upscatter soft photons on its thermal or non thermal  population of electrons. The main observational apperance which might help us to  determine the origin of the tail is its behavior at high energies.  The presence of high energy cutoff in this component will allow to distinguish between thermal and non thermal population of electrons and also  will allow to put constrains on possible influence of so called bulk motion comptonization on formation of the high energy component. INTEGRAL observatory is the only facility which can provide constrains on the physics of the high energy component of luminous accreting neutron  stars. It has abilities to study photon spectra at energies more than 100-200  keV with unprecedented accuracy. The limits obtained in the proposed study  will not be overcome by any existing and planning instruments for a long time. We suggest to perform 4 Msec-long observation of Sco X-1 split over two AOs  more than tripling the existing exposure. Among all possible galactic NS  systems in the appropriate spectral state Sco X-1 is by far the brightest  one (including high energy tail). This makes this object a must do target for the proposed study. [truncated! Please see actual data for full text]
DOI: 10.57780/esa-ltk08du
title: 8860136

description: OMC FF sequence ISOC V10 onwards: sequence of ff measurements with LED on/off followed by a DC cal.
DOI: 10.57780/esa-ltvzusa
title: 1320023

description: We ask for the continuation of our 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 including the hard X-ray variability of Sgr A* and to enable significant serendipitous science in the Galactic center region. We do not ask for data rights for any of the sources except for the Galactic Center. [truncated! Please see actual data for full text]
DOI: 10.57780/esa-lvccqt0
title: 8860169

description: OMC FF sequence ISOC V10 onwards: sequence of FF measurements with LED on/off followed by a DC cal.
DOI: 10.15468/dl.3xr5a9
title: Occurrence Download

description: A dataset containing 233 species occurrences available in GBIF matching the query:
{
 "and" : [
 "TaxonKey is Cassida azurea Fabricius, 1801",
 "HasGeospatialIssue is false",
 "HasCoordinate is true"
 ]
}

 The dataset includes 233 records from 52 constituent datasets; see https://api.gbif.org/v1/occurrence/download/0008424-250310093411724/datasets/export for details.
 
Data from some individual datasets included in this download may be licensed under less restrictive terms.
DOI: 10.57780/esa-lvtxuf7
title: 8860046

description: OMC FF sequence ISOC V10 onwards: sequence of ff measurements with LED on/off followed by a DC cal.
DOI: 10.57780/esa-m29nn58
title: 1420009

description: We ask for the continuation of the INTEGRAL Key Programme observations of 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 including the hard X-ray variability of Sgr A* and to enable significant serendipitous science in the Galactic center region. We do not ask for data rights for any of the sources except for the Galactic Center. [truncated! Please see actual data for full text]
DOI: 10.57780/esa-m2ve4lz
title: 0120244

description: Magnetically active stars are among the most ubiquitous high-energysources in the observable sky yet they have been studied predominantlyin the soft X-ray range below 10 keV where thermal coronal plasma is thepredominant source of photons. However both solar analogy and thepresence of strong non-thermal synchrotron emission from active stellarsources suggest the presence of a large population of non-thermal electrons out to MeV energies. They are expected to produce a strong non-thermal bremsstrahlung continuum above 10-20 keV. We proposehere a novel investigation to search for non-thermal hard X-ray emissionin stellar sources by combining results from several instruments on boardof INTEGRAL together with radio observations with the Very LargeArray. The results will be important to assess the role of acceleratedparticles in the primary energy release in stellar coronae as wellas their role in coronal heating. [truncated! Please see actual data for full text]
DOI: 10.57780/esa-m3864i7
title: 1770002

description: For the first time a periodicity has been found in arepeating FRB.The detection of a 16.35?0.18 day periodicity from the repeating FRB 180916.J0158+65 by the Canadian Hydrogen Intensity Mapping Experiment Fast Radio Burst Project (CHIME/FRB) has a strong impact on our knowledge of FRBs. So far no X-ray nor gamma-ray counteparts of FRBs have beendetected. The next burst activity for this source is predicted to happen from 2020-02-03 00:51 to 2020-02-07 22:35 with a peak around 2020-02-05 07:48. With this ToO we aim at finding a high energy counterpart of this burst activity characterizing for the first time the spectral and variability properties of such event. A detection at X-rays/soft gamma rays will allow to understand the nature of this class of FRB and to put a firm constraint on possible physical models invoked to explain the mysterious FRB phenomenon. [truncated! Please see actual data for full text]
DOI: 10.57780/esa-m57z931
title: 0310002

description: CP TOO follow-up observations of unknown X-ray novae.The trigger criteria are of two types. These types  define the number and the exposure times of the follow-up observations.
DOI: 10.57780/esa-m5txytl
title: 1670006

description: Coordinated observation of 3C273
DOI: 10.57780/esa-m6gddmj
title: 1020028

description: The gigahertz peaked spectrum (GPS) and compact steep spectrum radiosource PKS 1127-145 is a young radio-galaxy with a 300 kpc jet wasimaged by Chandra.  Chandra obsevations of the source revealed abright flat ~1.2 power-law spectrum which if extrapolatedto the IBIS/ISGRI energy range would allow a significant detection ofthe source.In this proposal we aim to detect the source spectrum above 10 keV. Thedetection of the source spectrum or even a simple detection could inprinciple discriminate among different scenarios for the production ofhigh-energy emission which in turn may have some bearing on theevolution of these objects. The source lies in an unexplored region of the INTEGRAL If accepted other extragalactic targets in the region would benefitas well from the increase in the exposure in this under-exposed regionof the sky. [truncated! Please see actual data for full text]
DOI: 10.57780/esa-m88hf9b
title: 1620016

description: Cas A and Tycho are remnants of a core-collapse and a type Ia supernova explosion respectively. Radioactive 44Ti  has been observed from these two relatively young supernova remnants and is believed to originate from the deep interiors of supernova explosions representing physical conditions that are otherwise difficult to explore. 44Ti  nucleosynthesis is assumed to occur in alpha-rich freeze-out from Si burning or NSE burning. The amount of 56Ni which also is produced in the supernova interior has been estimated indirectly  together the 44Ti/56Ni ratio is a key diagnostic of the inner processes in a supernova explosion. Here we propose deep observations of the sky region including both Cassiopeia A and Tycho in order to (1) advance Cas A 44Ti line results to sufficient quality for line shape and line ratio tests that reflect inner ejecta kinematics and (2) obtain sufficient exposure for Tycho to confirm the 44Ti signal reported from other instruments in the hard X-ray range. The SWIFT detection of 44Ti from Tycho a SN Ia remnant adds to the puzzle of 44Ti synthesis and the origins of cosmic 44Ca. 44Ti deposits radioactive energy in nebular-phase supernova remnants through positrons but the escape of positrons into interstellar space is an issue. Our planned observations will (3) constrain any local positron annihilation in the remnant itself thus possibly explain the disk faintness in 511 keV gamma-rays. Young supernova remnants are also believed to be predominant sources of cosmic rays. Our observations aim (4) to search for direct evidence signs of local cosmic-rays within the remnants such as nuclear de-excitation gamma-ray lines and continuum emission from Bremsstrahlung. [truncated! Please see actual data for full text]
DOI: 10.15468/dl.tr285s
title: Occurrence Download

description: A dataset containing 410 species occurrences available in GBIF matching the query:
{
 "and" : [
 "Country is Netherlands",
 "License is CC-BY 4.0",
 "TaxonKey is Cricetidae"
 ]
}

 The dataset includes 410 records from 12 constituent datasets; see https://api.gbif.org/v1/occurrence/download/0008425-250310093411724/datasets/export for details.
 
Data from some individual datasets included in this download may be licensed under less restrictive terms.
DOI: 10.57780/esa-mbx3clr
title: 0420032

description: The peculiar dipping Low-Mass X-ray Binary EXO 0748-676 represents a paradigm for many dipping LMXB phenomena andhas been  extensively studied in X-rays (E < 10 keV) by means of many satellites.We propose to perform for the first time an extensive study of its high energy emissionin order to better understand its geometry (presence and extension of anAccretion Disk Corona and of a thermal halo) temporal properties (e.g. neutron star spin periodmeasured at high energies QPOs etc.) and variability (eclipses dips flares thermonuclear bursts etc.). Gotz et al. (2006) reported the results from an INTEGRAL observation of thesource which however was detected at large off-axis angles making detailedstudies difficult.In order to fully exploit the sensitivity of the INTEGRAL instrumentswe propose to observe this source for a total of 2x200 ks (hexagonal dithering) as a primary target. [truncated! Please see actual data for full text]
DOI: 10.57780/esa-mcqb4he
title: 1870011

description: Integral TOO observations of  MAXI J0903-531
DOI: 10.57780/esa-mdpgfk8
title: 1120011

description: We propose to perform a long INTEGRAL observation of 700 ks of the Seyfert 1 galaxy NGC 5548 simultaneously with an already accepted XMM-Newton pointing during a unique and very large multi-wavelength monitoring of this source. The high energy capabilities of INTEGRAL will permit: 1) to complete the long-term light curve of the 20--60 keV flux of NGC 5548 and 2) to provide the best possible hard X-ray/soft gamma-ray spectrum  of this object. As experienced from a previous very successful campaign led by our group on the Seyfert 1 Mrk 509 we need precise knowledge of the hard X-ray/soft gamma-ray band.  On the one hand  the hard X-ray/soft gamma-ray light curve is of prime importance for the characterization of the ionizing radiation critical information for an accurate time-dependent modeling of the warm-absorber properties that will be observed in detail with XMM-Newton.  On the other hand the hard X-ray/soft gamma-ray spectrum is crucial to constrain the physical parameters of the Comptonizing corona responsible for the bulk of the X-ray emission.  When combined with XMM-Newton lower-energy information it allows also to correctly disentangle the different spectral components present in the UV soft X medium X-ray and gamma-ray bands and in consequence to better understand their origins. [truncated! Please see actual data for full text]
DOI: 10.57780/esa-mdtwr5x
title: 8860187

description: Crab-2009 August: 5x5 pattern (wide: 2.33 deg between points)
DOI: 10.57780/esa-mjrdcce
title: 8860290

description: Crab 2013: SPI/IBIS 5x5 wide rev 1268 and 1269
DOI: 10.57780/esa-mkllx72
title: 0520001

description: The Galactic bulge region is a rich host of variable X-ray and gamma-ray point sources.In AO-3 and AO-4 we have been monitoring this region with one hexagonal observation approximately every 3 days whenever it was visible by INTEGRAL. Because of the high scientific return and to preserve the continuity with respect to past observations of this ever-changing regionwe suggest to continue our successful observing program. As a service to the scientificcommunity we make the IBIS/ISGRI and JEM-X light curves both in two energy bands perscience window and per hexagonal observation as well as the mosaic images per hexagonalobservation publicly available through the web as soon as possible after theobservations have been performed. Any interesting source behaviour which emerges from ourobservations will be announced promptly so that rapid follow-up by the community ispossible. Our team consists of scientists with expertise on a large range of topics. We alsointend to do a more in-depth analysis (spectra bursts flares etc.) of sources of particular intereston short and long time scales. These sources include bright and relatively faint X-raytransients X-ray bursters persistent neutron star and black-hole candidate binarieshigh-mass X-ray binaries etc.. [truncated! Please see actual data for full text]
DOI: 10.57780/esa-mksbrl5
title: 1020006

description: We request an INTEGRAL observation of 500 ksec of the bright Seyfert 2 galaxy NGC 2992. Analysis using the latest OSA-9 software of the INTEGRAL observations in 2005 shows a cut-off power law consistent with previous observations (e.g. by BeppoSAX). At the same time NGC 2992 has been shown to be the most variable Seyfert at hardest X-rays on months time-scale. Observing NGC 2992 again after 8 years enables us to study this Seyfert 2 galaxy at a possibly different flux state and in a different spectral state. The observations can help to clarify whether super massive black holes follow a similar spectral behaviour as Galactic black hole systems.INTEGRAL offers the unique possibility to study the physics involved in absorbed AGN and even enables us to study the connection between flux variation high-energy cut-off reflection component and iron fluorescenceline. The variation in flux over the time of the observation in various energy bands can reveal the geometry of this source. In the case that the state of the source is similar as 7 years ago the observation will help to further constrain the high energy spectrum of this source. A simultaneous 10 ks XMM-Newton observation will measure precisely the amount of absorption in the line of sight the strength of the iron K-alpha line and will allow us to determine the reflection component to a precision of (Delta R) ~ 0.3. [truncated! Please see actual data for full text]
DOI: 10.57780/esa-mmfs90w
title: 8860110

description: AOCS calibration for rev 446
DOI: 10.57780/esa-mnadujt
title: 8860300

description: OMC FF sequence ISOC V10 onwards: sequence of ff measurements with LED on/off followed by a DC cal.
DOI: 10.57780/esa-mnm50pj
title: 0620028

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 scenario in 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-mo3q0oq
title: 0399839

description: Galactic Plane Survey for AO 03 and Pattern 39
DOI: 10.57780/esa-mq1gf24
title: 1120009

description: In this AO we propose to observe for 700 ksec the brightest broad line radio galaxy (IGR J21247+5058) in the hard X-ray sky. We request a joint 10 ksec observation with XMM ideally covering the central part of the INTEGRAL pointing  two Swift/XRT observations of 10 ksec each will also be performed at the beginning and at the end of the INTEGRAL measurement  we will also have a daily radio monitoring of the source at 15 GHz using the AMI telescope. The aim of this proposal is to obtain high quality simultaneous coverage over a broad energy range in order to characterise both the low and high energy spectral param- eters and the weak reprocessing features of the source also providing further monitoring of this peculiar object which has complex and variable absorption at odds with its type 1 classification. The simultaneity of the XMM and INTEGRAL observations together with the Swift/XRT measurements will allow us to assess the nature of the variability in this source as well as to place stringent constraints on two important high energy parameters: the high energy cut-off and the Compton reflection hump above 10 keV. Compared with previous data this joint observation can shed light on the nature of a bright and quite peculiar radio galaxy. [truncated! Please see actual data for full text]