JOINT XMM-HST PROGRAMS

For XMM-Newton's Cycle 18 and HST's Cycle 26/27, the XMM-Newton Observing Time Allocation Committee (OTAC) met in the fall of 2018 and reviewed their proposals. The following six joint XMM-Newton proposals (listed below) have been approved for execution in HST Cycle 26/27. These observations have been loaded with the current Cycle 26 programs.

Discovering the X-ray Broad Line Region in AGN

Elisa Costantini 
Space Research Organization Netherlands
Program ID: 15669

Thanks to high resolution spectroscopy, the X-ray emitting broad line region has been recently discovered and studied in few bright type 1 Seyferts. We propose to observe for 120 ks the bright AGN Mrk110, simultaneously with HST-COS. The goal is to model for the first time the panchromatic broad line region emission in a Narrow Line Seyfert~1 galaxy. We will use the broad lines from the optical, UV and X-rays in a global modeling that will characterize the stratification, extend and ionization of the broad line emitting region, whose Xray extension still awaits a full characterization.

Studying Six Galaxy Clusters to be Used as Gravitational Lense Telescopes

Hans Boehringer 
University Observatory, Ludwig-Maximilians-University, Munich
Program ID: 15670

The most massive galaxy clusters are extremely valuable study objects for a wide range of astrophysical and cosmological studies. In our completed all-sky X-ray cluster survey we found 6 rare, massive galaxy clusters (M500 greater than 6.4 x 10e14 Msun) in the redshift range z = 0.25 to 0.5 (sweet spot for gravitational lensing studies), which have not been observed in X-ray pointed observations so far (one has a short XMM exposure). We propose these objects for XMM-Newton and the two most interesting systems for HST observations, with a main goal to characterise their properties for lensing studies and their use as gravitational lensing telescopes. In addition these observations complete an important sample of massive clusters to be used for a range of cosmological studies.

Unveiling the Nature of Fossil Groups with XMM-HST II: Reducing Variance

Renato Dupke
Eureka Scientific Inc.
Program ID: 15671

Fossil groups (FGs) present a puzzle to theories of structure formation. Despite the low number of bright galaxies, their high velocity dispersions and high T X seem to indicate cluster-like potential wells. Their measured c200 are high indicating early formation epochs, in contradiction with the observed lack of expected large cool cores. We have proposed a discriminatory test, using the intracluster light to mass ratio (ICLf/M) in FGs, using XMM and HST. The pilot study was successful and suggests that FGs are not merging and show high ICLf/M ratios in comparison to relaxed systems. We propose to increase the sample of bonafide FGs complementing XMM and HST archived observations to account for sample variance, allowing us to reliably constrain their formation mechanisms and ages.

Catching AGN in Deep Minimum States to Unveil Their Core Environment

Norbert Schartel
European Space Agency - ESTEC
Program ID: 15672

The deep minimum state of AGN is characterized by a strongly suppressed or even absent primary continuum. As the continuum disappears weak spectral features like relativistic iron lines or narrow soft X-ray emission lines from ionised plasmas become highly significant and their parameters can be determined. Therefore deep minimum states offer unique possibilities to investigate in detail the physics of the reprocessed components in AGN, including the immediate vicinity of the supermassive black hole. Applying our experience (several deep minimum observations) we propose 2 triggered 10ks XMM snapshot, one 80ks XMM follow-up simultaneous with one 80ks NuSTAR one 2-orbit HST observation of an AGN in deep minimum state.

Shining light on obscuring outflows in AGN

Jelle Kaastra
Space Research Organization Netherlands
Program ID: 15673

AGN can be obscured by gas streams close to the black hole that shield remote regions from ionising radiation. We witnessed such an event in NGC 5548 and NGC 3783 where 90% of the soft X-rays are blocked by a dense gas stream close to the BLR. Our joint observations with XMM-Newton, NuSTAR and HST/COS showed UV broad absorption lines associated with the X-ray absorption and allowed us to characterise this unique obscuration event completely. We propose to investigate a similar event in another Seyfert 1 using the same instruments. Swift monitoring (98 ks) will be used to find the event, which will be characterised by joint ToO observations with XMM-Newton (150 ks), HST/COS (4 orbits) and NuSTAR (50 ks).

A new adventure of the musketeer PSR B1055-52

Bettina Posselt
The Pennsylvania State University
Program ID: 15676

The nearby, middle-aged neutron star PSR B1055-52, one of the so-called Three Musketeers, has been observed once by XMM-Newton in 2000 resulting in a detailed phase-resolved spectral analysis. Chandra observations in 2012 show spectral changes and an apparent greater than 30% flux decrease with respect to the 2000 XMM-Newton observation. These changes are too large to be due to cross-calibration problems. We propose new XMM-Newton observations to probe the apparent spectral changes. Using a better suited instrument mode than the 2000 observations, we will also be able to measure more accurately the magnetospheric spectral component and relate it to the radio and gamma-ray pulse profiles. Furthermore, we will search for phase-dependent absorption features in the new epoch data.

For XMM-Newton's Cycle 17 and HST's Cycle 25/26, the XMM-Newton Observing Time Allocation Committee (OTAC) met in the fall of 2017 and reviewed their proposals. The following five joint XMM-Newton proposals (listed below) have been approved for execution in HST Cycle 25/26. These observations have been loaded with the current Cycle 25 programs.

Catching AGN in Deep Minimum States to Unveil Their Core Environment

Norbert Schartel
European Space Agency - ESTEC
Program ID: 15439

The deep minimum state of AGNs is characterized by a strongly suppressed or even absent primary continuum. As the continuum disappears weak spectral features like relativistic iron lines or narrow soft X-ray emission lines from ionised plasmas become highly significant and their parameters can be determined. Therefore deep minimum states offer unique possibilities to investigate in detail the physics of the reprocessed components in AGN, including the immediate vicinity of the supermassive black hole. Applying our experience (several deep minimum observations) we propose 2 triggered 10ks XMM snapshot, one 80ks XMM follow-up simultaneous with one 80ks NuSTAR one 2-orbit HST observation of an AGN in deep minimum state. We will identify deep minimum states mainly based on Swift and XMM-Newton slews.

X-ray and UV monitoring of the extraordinary changing-look AGN Mrk 1018

Mirko Krumpe
Leibniz-Institut fur Astrophysik Potsdam (AIP)
Program ID: 15440

We propose two quasi-simultaneous observations of XMM (each 65 ks) and HST (each 2 orbits) to understand the ongoing changes of changing-look AGN Mrk 1018. Optical monitoring revealed that the dramatic dimming phase stopped, suggesting that the accretion disk is in a major reconfiguration phase. The combined deep exposure will reveal which spectral components have changed since a high S/N XMM spectrum was taken during the bright phase a few years ago. Comparing the two AO17 observations will allow us to look for spectral changes on half-year timescales. These two XMM observations will fill the gaps of our already accepted low S/N Chandra monitoring program on Mrk 1018. The joint HST observations will allow us to establish the states of the accretion disk and how this connects to the X-ray corona.

Follow-up Observation of a Hyperluminous Intermediate-mass Black Hole Candidate

Dacheng Lin 
University of New Hampshire
Program ID: 15441

Intermediate-mass black holes (IMBH, ~10^2-10^5 msun) have been long sought after because they are associated with several important astrophysical processes. The best IMBH candidates are hyperluminous off-nuclear X-ray sources (HLXs) with LX>10^41 erg/s, but very few are known. We have identified a new HLX candidate (LX~10^43 erg/s), at an offset of 11.6" (12 kpc) from the center of its host galaxy (D L=247 Mpc). We request a deep (60 ks) XMM-Newton observation of the source in AO17 to measure its flux and spectral evolution while it is in the decay phase of a prolonged outburst, in order to demonstrate its IMBH nature and confirm our tidal disruption event explanation for the outburst. An HST orbit is also requested to confirm that our source is in a star cluster.

GSN 069: a recent AGN re-activation or a long-lasting Tidal Disruption Event ?

Giovanni Miniutti 
Centro de Astrobiologia (CSIC/INTA) Inst. Nac. de Tec. Aero.
Program ID: 15442

We request an XMM-Newton and HST/STIS observation of GSN 069, an ultra-soft, unabsorbed, highly variable X-ray source optically classified as a Seyfert 2 AGN. Its high Eddington ratio (0.5) makes GSN 069 an exceptional high Eddington ratio 'true Seyfert 2 galaxy' candidate. The data so far suggest two possible interpretations: 1) a recent re-activation of the AGN after a period of low activity or quiescence or 2) an unusual (but not unique) long-lived outburst due to a Tidal Disruption Event (TDE). With our joint XMM/HST program we aim at clarifying the nature of this most exceptional source and derive constraints on the formation and evolution of BLR, disc winds, and AGN X-ray coronae in the first scenario, or on the nature of rare sustained TDEs in the second.

Unveiling the Nature of Fossil Groups of Galaxies with XMM-Newton-HST

Renato Dupke
Eureka Scientific Inc.
Program ID: 15443

Fossil groups present a puzzle to theories of structure formation. Despite the low number of bright galaxies, their high velocity dispersions and high T X seem to indicate cluster-like gravitational potential wells. The measured concentration parameters seem to be high indicating early formation epochs but some recent observations contradict that scenario. We propose a discriminatory test, using intracluster light to mass ratio, combining short XMM and HST observations for a classic massive fossil group. We will use a newly developed method for measuring ICL that is independent of arbitrary assumptions about light distribution and that has provided new robust results. This test will allow us to set independent constraints on formation mechanisms and ages of these peculiar (but numerous) systems.

For XMM-Newton's Cycle 16 and HST's Cycle 25, the XMM-Newton Observing Time Allocation Committee (OTAC) met in the fall of 2016 and reviewed their proposals. The following three joint XMM-Newton proposals (listed below) have been approved for execution in HST Cycle 25. These observations have been loaded with the current Cycle 24 programs.

Understanding the Super-Eddington phase in a Decade-long Tidal Disruption Event

Dacheng Lin
University of New Hampshire
Program ID: 14905

We have discovered a decade-long X-ray tidal disruption candidate, which recent observations suggest to be still in the super-Eddington accretion phase but with sporadic dramatic spectral softening. We request three XMM-Newton monitorings in AO16 on this target, which is unique for study of the super-Eddington accretion onto supermassive black holes. The goals are to confirm its still being in the super-Eddington accretion phase and to measure the spectral softening occurrence rate, allowing us to determine whether the spectral softening is due to transient high-speed warm absorbers or state transition. We also request an HST orbit to help confirm the nuclear origin of the event and study its environment.

UV irradiation of the Earth-sized planets orbiting TRAPPIST-1

Peter Wheatley 
The University of Warwick
Program ID: 14906

The remarkable discovery of a system of three Earth-sized potentially-habitable planets transiting the ultra-cool dwarf TRAPPIST-1 provides an unprecedented opportunity for detailed study of the atmospheres of terrestrial exoplanets. Our analysis of an archival XMM-Newton observation of the star revealed XUV radiation that was fifty times stronger than assumed in a theoretical study of the planetary atmospheres, with enough XUV irradiation to profoundly modify and perhaps entirely strip those atmospheres. Here we propose a longer XMM-Newton observation that will cover a full spin cycle of the star and more accurately define the XUV irradiation of the exoplanets. This is an essential step in assessing the habitability of these and similar exoplanets around ultra-cool dwarfs.

Probing the merger-induced feedback scenario in hyper-luminous quasars

Luca Zappacosta 
INAF, Osservatorio Astronomico di Roma
Program ID: 14908

We are following up through multiwavelength observations the WISSH sample of hyperluminous MIR-selected Type 1 quasars at z~2.5-3.5. In these objects we expect powerful quasar feedback and galaxy mergers to manifest themselves in full force. We are finding the WISSH quasars to exhibit a mixture of two populations with powerful winds in different gas phases (OIII or CIV). They also seem to show a dichotomy in their X-ray luminosities and UV/X-ray slope. We propose here XMM and HST observations of three WISSH quasars showing powerful OIII outflows in order to establish whether (i) they have higher X-ray-to-MIR and X-ray-to-UV luminosity ratios compared to the CIV-wind population and (ii) powerful quasars in the blow-out phase are linked to mergers.

For XMM-Newton's Cycle 15 and HST's Cycle 24, the XMM-Newton Observing Time Allocation Committee (OTAC) met in the fall of 2015 and reviewed their proposals. The following four joint XMM-Newton proposals (listed below) have been approved for execution in HST Cycle 24. These observations have been loaded with the current Cycle 23 programs.

The global view of the ionized outflows in NGC 4051

Dr. Elisa Costantini
Space Research Organization Netherlands
Program ID: 14479

We propose to observe the bright active galactic nucleus NGC 4051 for 120 ks jointly with HST and Astro-H. This source hosts one of the most extraordinary multi-phase ionized outflows. For the first time, we will acquire a high-resolution spectrum of the low, medium and highly ionized outflow in a low-mass black hole. We will study the connection between the X-ray and UV absorber and the disk winds mapping the ionization structure, kinematic behavior and relative abundance.

Joint XMM-Newton and HST study of the magnetic weak- wind O-star HD 54879

Dr. Wolf-Rainer Hamann
Observatoire de Strasbourg
Program ID: 14480

Current massive-star astrophysics struggles with a number of urgent questions: what are the true mass-loss rates, what is the role of magnetic fields, how are X-rays produced? HD54879 provides an important laboratory to study these questions. While a strong magnetic field (2.1 ,kG) has been recently detected in this star, it otherwise exhibits a normal spectrum of O9.7 main sequence type. We propose joint XMM and HST observations of HD54879. Analysis of the UV spectrum will establish the parameters of the cool stellar wind, while from the XMM data the hot plasma component will be studied. The new observations will establish a gauge for stellar wind theory and provide a template X-ray spectrum for magnetic massive stars with weak wind.

Shining light on obscured AGN outflows

Dr. Jelle Kaastra
Space Research Organization Netherlands
Program ID: 14481

AGN can be obscured by gas streams close to the black hole that shield remote regions from ionising radiation. We witnessed such an event in NGC 5548 where 90% of the soft X-rays are blocked by a dense gas stream close to the BLR. Our joint observations with XMM-Newton, NuSTAR and HST/COS showed UV BAL lines associated with the X-ray absorption and allowed us to characterise this unique obscuration event completely. We propose to investigate a similar event in another Seyfert 1 using the same instruments. Swift monitoring will be used to find the event, which will be characterised by joint ToO observations with XMM-Newton (150 ks), HST/COS (4 orbits) and NuSTAR (50 ks).

A long, broad and high resolution look at NGC 3783: joint with ASTRO-H

Dr. Jelle Kaastra
Space Research Organization Netherlands
Program ID: 14482

We propose a 160 ks observation of the bright Seyfert 1 galaxy NGC 3783 using XMM-Newton and 2 HST- COS orbits. This will overlap with a 100 ks PV phase observation with Astro-H. We will study the warm absorber in unprecedented detail: enumerate the ionization components, measure outflow speeds, and search for new high ionization components. We will measure the broad-band spectrum more accurately than ever before, which will allow better determination of the broad iron line shape and black hole spin. We will search for variability both within the observation and over historical timescales. These observations will provide the highest spectral resolution over the largest relevant bandwidth; our findings will be applicable to all AGN outflows and broad-band spectra.

XMM and HST Target of Opportunity Observations of Tidal Disruption Events

Dr. Andrew Levan
The University of Warwick
Program ID: 14483

Tidal disruption events (TDEs), where a star is disrupted while passing close to a black hole, enable a view of accretion onto supermassive objects from quiescence to super-Eddington rates, on a timescale of a few years. Here we propose to characterise the spectral and temporal properties two TDEs found in AO15. As part of a comprehensive multiwavelength campaign we will use XMM-Newton and HST to map either side of the expected hot black-body peak; search for evidence of non-thermal components; track the cooling of the event and study the long and short timescale variability of the sources. In doing so we will create exquisite, panchromatic pictures of these extreme events.

A collision reversal in HD5980

Dr. Yael Naze
Universite de Liege
Program ID: 14476

HD 5980 provides a unique laboratory for studying the properties of wind-wind collisions. It contains one of only two binary systems having a WR-star in orbit with a LBV. The latter star has been observed to undergo major changes in its wind structure over the past 35 years, implying changes in the geometry and emitting conditions of the wind-wind collision region. Ten years ago, when the LBV wind was very strong, XMM observations revealed X-ray emission consistent with the shock cone wrapping around the WR component. Since then, the LBV wind strength has significantly declined, implying that the collision shock cone may be inverting its orientation. The objective of this proposal is to obtain X-ray coverage of this never before observed phenomenon.

UV to hard X-ray spectroscopy of the prototype disk wind quasar, PDS 456

Dr. James Reeves
University of Maryland Baltimore County
Program ID: 14477

PDS 456, the most luminous nearby AGN, is now recognised as the prototype ultra fast outflow. Our recent XMM-Newton and NuSTAR campaign on PDS 456 established the presence of a fast (0.3c), wide angle disk wind, sufficient to provide significant mechanical feedback into its host galaxy. The new RGS data have revealed the presence of variable, broad soft X-ray absorption lines from the disk wind, which may be associated to the partial covering absorber. Here we propose for 2x80 ks XMM-Newton observations of PDS 456 and a two orbit HST/COS snapshot which will simultaneously measure the wind in the UV and X-rays. The requested observations will be concurrent with a likely Astro-H observation during 2016. For the first time we will obtain high resolution coverage of the wind from the UV to hard X-rays.

Catching AGN in Deep Minimum States to Unveil Their Core Environment

Dr. Norbert Schartel
XMM-Newton SOC
Program ID: 14478

The deep minimum state of AGNs is characterized by a strongly suppressed or even absent primary continuum. As the continuum disappears weak spectral features like relativistic iron lines or narrow soft X-ray emission lines from ionised plasmas become highly significant and their parameters can be determined. Therefore deep minimum states offer unique possibilities to investigate in detail the physics of the reprocessed components in AGN, including the immediate vicinity of the supermassive black hole. Applying our experience (several deep minimum observations) we propose 2 triggered 10ks XMM snapshot, one 80ks XMM follow-up simultaneous with one 80ks NuSTAR one 2-orbit HST observation of an AGN in deep minimum state. We will identify deep minimum states mainly based on Swift and XMM-Newton slews.

For XMM-Newton's Cycle 14 and HST's Cycle 23, the XMM-Newton Observing Time Allocation Committee (OTAC) met in the fall of 2014 and reviewed their proposals. The following four joint XMM-Newton proposals (listed below) have been approved for execution in HST Cycle 23. These observations will be processed during the normal HST cycle ingest after the HST Telescope Allocation Committee (TAC) meets in June of 2015 with results released to the community by late-June.

Tracking Down the Ionized Outflow of NGC 7469

Prof. Ehud Behar
Technion – Israel Institute of Technology University
Program ID: 14054

Using a multiwavelength campaign on NGC 7469, led by XMM-Newton, HST, Swift, NuSTAR, and optical, we propose to achieve new physical insights into the enigmatic AGN winds, by obtaining the deepest ever RGS spectrum of this highly- accreting source. It will allow us to determine the accurate ionisation and chemical structure of the wind. Using EPIC and RGS, we will measure the response of the outflow to continuum variations, which combined with HST/COS data will unambiguously determine the location, and abundances of the outflow components. Our team pioneered this approach, and applied it successfully (14 refereed papers) to Mrk 509 that featured only a multi-year response. The unique properties of NGC 7469 make it the ideal candidate to respond on shorter, better-monitored time scales.

Changes in the X-ray irradiation of an ultraluminous X-ray source

Dr. Fabien Grise
Observatoire de Strasbourg
Program ID: 14057

Optical emission observed from ultraluminous X-ray sources (ULXs) comes from the irradiated disk and the donor star. Disentangling the two components has always been an unsolved problem. We have discovered that the ULX NGC 1313 X-2 switches between two distinct X-ray spectral/luminosity states on long timescales, ~ 6--10 weeks.
This makes it an ideal laboratory to study the effects of variable X-ray irradiation on the disk and donor star. We propose a multiband study of NGC 1313 X-2 from near-IR to X-rays, with XMM, HST and Swift. We will measure the contribution of X-ray reprocessing to the optical emission and determine whether irradiation correlates with disk winds.

State transitions of the ULX in M83

Dr. Roberto Soria
International Centre for Radio Astronomy Research
Program ID: 14059

We study a transient ultraluminous X-ray source (ULX) in M83, which went into outburst in 2010 and is now evolving towards the luminosity range of ordinary stellar-mass black holes. We propose an XMM-Newton and HST study: a) to model the spectral state evolution during the decline, and discover how the ULX regime is linked to the sub-Eddington accretion states of Galactic BHs; b) to determine or constrain the mass of the BH, from X-ray spectroscopy; c) to quantify the properties of the irradiated disk, and its response to variable X-ray illumination.

A huge ULX bubble in NGC 5585

Dr. Roberto Soria
International Centre for Radio Astronomy Research
Program ID: 14060

Accreting black holes release their power through radiation and/or jets. We have discovered an ultraluminous X-ray source (ULX) in the nearby galaxy NGC 5585, surrounded by a large (diameter ~300 pc) ionized nebula. We propose a joint XMM- Newton and HST study of this source. With XMM-Newton, we will determine the radiative power of the ULX, its spectral and time variability properties, and constrain its mass. With HST, we will image the nebula, determine whether it is a jet-inflated ULX bubble, measure its kinetic power and source age, and search for an optical counterpart to the black hole.

For XMM-Newton's Cycle 13 and HST's Cycle 22, the XMM-Newton Observing Time Allocation Committee (OTAC) met in the fall of 2013 and reviewed their proposals. The following six joint XMM-Newton proposals (listed below) have been approved for execution in HST Cycle 22. These observations will be processed during the normal HST cycle ingest after the HST Telescope Allocation Committee (TAC) meets in June of 2014 with results released to the community by late-June.

Feedback in action in the type 1 Seyfert IZw 1

Dr. Elisa Costantini
Netherlands Institute for Space Research
Program ID: 13811

We propose simultaneous 200 ks XMM-Newton-RGS and HST-COS observations of the narrow line Seyfert1 IZw1. We will study the connection between the X-ray and UV absorber, mapping the ionization structure, kinematic behavior and elemental abundances. Finally we will quantify the AGN feedback by directly measuring the metal enrichment by C, N, O, and Fe and the kinetic luminosity of the outflow.

Tomography of the innermost regions of NGC 985

Dr. Jacobo Ebrero
Netherlands Institute for Space Research
Program ID: 13812

AGN mass outflows inject enormous amounts of matter and energy into the interstellar medium of the host galaxy. Their location, structure, and importance as contributors to cosmic feedback processes are not yet fully understood. We propose to observe the Seyfert 1 galaxy NGC 985 with XMM-Newton for 240 ks using RGS as the prime instrument in order to accurately characterize the different ionized phases and kinematic components of the warm absorber. Together with HST/COS we will study the connection between the X-ray and UV absorbers and put stringent limits on the location of these winds in the context of the unification model of AGN.

Mapping the Broad-band Spectrum of a New Candidate Intermediate Mass Black Hole

Dr. Sean Farrell
The University of Sydney
Program ID: 13813

We request joint XMM-Newton & HST observations of a new intermediate mass black hole candidate in the galaxy LEDA 87326 to map the broad-band spectral energy distribution from X-ray to near-IR. Previous observations with the XMM-Newton EPIC and OM cameras detected an X-ray source with an observed 0.2-10 keV luminosity of 6E41 erg/s, with the X-ray spectrum dominated by a hard power law and the UV/optical data consistent with thermal emission from a cool (~0.08 keV) accretion disc. The high X-ray luminosity and low disc temperature imply a black hole mass > 4000 Msun. By observing this source simultaneously with XMM-Newton and the HST we will confirm that the observed optical emission is from an accretion disc and determine whether any reprocessing in the outer disc is present.

The rise of an ionized outflow in the X-ray and UV spectra of the NLS1 Mrk 335

Dr. Anna Lia Longinotti
ESAC
Program ID: 13814

We propose to obtain contemporaneous high resolution spectroscopy of the Narrow Line Seyfert 1 Galaxy Mrk 335 with triggered XMM-Newton/RGS (130 ks) and HST/COS (7 orbits) observations with the aim of studying the properties of the ionized outflow that has recently been discovered in archival data. XMM/RGS spectra obtained during an intermediate flux state (June 2009) revelead the presence of multi-component ionized gas outflowing at ~5000 km/s. In HST/COS data taken a few months later (Oct 2009-Feb 2010) we found evidence for smooth, broad and weak CIV absorption. The global behavior of the gas in both bands can be explained by variation of the covering factor and/or column density, possibly due to transverse motion of absorbing clouds at Broad Line Region scale.

Early evolution of AGN X-ray coronae and the X-ray, BLR, disc-wind connection

Dr. Giovanni Miniutti
Centro de Astrobiologia
Program ID: 13815

We request a quasi-simultaneous XMM-Newton and HST/STIS observation of GSN 069, a high-Eddington ratio true/unabsorbed Seyfert 2 galaxy candidate with ultra-soft X-ray spectrum. From our study of previous X-ray/optical spectra and of UV photometric data, we infer that the lack of BLR in this peculiar object may be attributed to ether (i) the lack of hard X-ray emission or (ii) an evolutionary scenario in which the BLR are just forming. Recent Swift pointings have revealed the emergence of hard X-rays in GSN 069, making the proposed observation highly timely. GSN 069 may represent a true Rosetta stone with which to follow the formation and early evolution of the X-ray corona and to study the connection between X-rays and the BLR/disc-wind system.

Characterizing the high-energy properties of a highly magnetized star

Dr. Yael Naze
University de Leige
Program ID: 13629

CPD-28 2561 is the only known magnetic O-star without high-energy observations. However, because of the particular geometry of this object, it represents a crucial step towards a full understanding of the dynamic magnetospheres of high-mass stars. We propose to fill this gap by observing it in X-rays as well as in UV, both with high-resolution and with a monitoring to sample crucial phases. These complementary data will help us constrain the energetics, shock physics and 3D structure of the magnetosphere of this unique object.

For XMM-Newton's Cycle 12 and HST's Cycle 21, the XMM-Newton Observing Time Allocation Committee (OTAC) met in the fall of 2012 and reviewed their proposals. The following five joint XMM-Newton proposals (listed below) have been approved for execution in HST Cycle 21. These observations will be processed during the normal HST cycle ingest after the HST Telescope Allocation Committee (TAC) meets in May of 2013 with results released to the community by late-May.

Monitoring the awakening of the dormant SMBH at the center of our galaxy

Dr. Nicolas Grosso
Observatoire de Strasbourg
Program ID: 13403

The recently discovered G2 dense dusty gas cloud, infalling towards the dormant SMBH at the center of our galaxy SgrA*, should reach its pericenter in September 2013. The X-ray luminosity of SgrA* is expected to increase significantly at this period and the fragmentation of this cloud should lead to an enhanced activity period over several months/years. Therefore, we propose a large program to monitor SgrA* during the course of the G2 cloud near its pericenter passage and after this event, combining the XMM-Newton high-throughput with several multi-wavelength observations with ground-based telescopes and satellites. This will offer us an unique opportunity to study accretion events on a dormant SMBH and its (re-)activation process.

Deciphering AGN outflows: multiwavelength monitoring of NGC 5548

Dr. Jelle Kaastra
Netherlands Institute for Space Research (SRON)
Program ID: 13184

AGN outflows couple supermassive black holes to their environments. Using an ambitious multiwavelength campaign on NGC 5548, (XMM-Newton, HST, Swift, and optical) we propose to achieve a new level of physical understanding for these enigmatic winds by obtaining the deepest RGS spectrum of any AGN, allowing us to determine the ionisation structure of the gas. Using EPIC data we will measure the response of the outflow to continuum variations, which combined with HST/COS data determines unambiguously the location and tomography of the outflow components. Time-dependent UV and X-ray continuum variations will constrain the geometry and physics close to the black hole. Our team pioneered this approach, and recently applied it successfully (12 refereed papers) to Mrk 509.

Probing Black Hole Disk Atmospheres with EPIC and RGS Observations of 4U 1957+11

Dr. Michael Nowak
MIT
Program ID: 13380

We propose contemporaneous XMM-Newton and HST-COS observations of the black hole candidate 4U1957+11. We plan to search both the X-ray and UV spectra for evidence of a blue-shifted, magnetized wind, similar to that observed in high-resolution X-ray spectra of GRO J1655-40.

Catching AGN in Deep Minimum States to Unveil Their Core Environment

Dr. Norbert Schartel
XMM-Newton SOC, ESA
Program ID: 13387

The deep minimum state of AGNs is characterized by a strongly suppressed or even absent primary continuum. As the continuum disappears weak spectral features like relativistic iron lines or narrow soft X-ray emission lines from ionised plasmas become highly significant and their parameters can be determined. Therefore deep minimum states offer unique possibilities to investigate in detail the physics of the reprocessed components in AGN, including the immediate vicinity of the supermassive black hole. Applying our experience (several deep minimum observations) we propose two triggered 10ks XMM snapshot, one 80ks XMM follow-up and one HST (2 orbit) observation of an AGN in deep minimum state. We will identify deep minimum states based on Swift and XMM-Newton slew observations. This is a HST Disruptive ToO.

An XMM-Newton+HST study of the likely most X-ray luminous z>=0.9 galaxy cluster

Dr. Tim Schrabback
Bonn University
Program ID: 13493

We propose XMM-Newton+HST observations of the new, extremely X-ray luminous cluster ClGJ120959.0+495352 (z=0.90), discovered through our combined search of RASS and SDSS data. Optical and SZ data suggest that it is an excellent candidate for a very massive, dynamically relaxed cooling-core cluster, which are extremely rare at high z. The XMM-Newton data will provide the first resolved X-ray imaging of the system to confirm its dynamical state and constrain both the temperature profile and global cluster properties. The HST data will provide complementary constraints on the cluster mass and dynamical state from strong and weak lensing, enabling the comparison to scaling relations and the assessment if the cluster’s discovery is in line with standard cosmological expectations.

For XMM-Newton's Cycle 11 and HST's Cycle 20, the XMM-Newton Observing Time Allocation Committee (OTAC) met in the fall of 2011 and reviewed their proposals. The following six joint XMM-Newton proposals (listed below) have been approved for execution in HST Cycle 20. These observations will be processed during the normal HST cycle ingest after the HST Telescope Allocation Committee (TAC) meets in May of 2012 with results released to the community by mid-June.

The Stellar Population Around the Intermediate Mass Black Hole ESO 243-49 HLX-1

Dr Sean Farrell
The University of Sydney
Program ID: 12979

We request joint XMM-Newton and HST observations of the best intermediate mass black hole candidate HLX-1. Recent HST and Swift observations found the broadband spectral energy distribution was well described by an irradiated accretion disc plus a stellar population. However, degeneracies in the models resulted in two acceptable solutions with dramatically different parameter values. We request two observations to be performed with XMM-Newton and the HST at different X-ray luminosities in order to break these model degeneracies using the variability of the disc emission. With these 2 - 5 orbit observations we will be able to determine the nature of the environment around the black hole, test formation theories for HLX-1, and rule out beaming as the origin of the extreme luminosities.

XMM-Newton Target of Opportunity of Tidal Disruption Events

Dr Andrew Levan
University of Warwick
Program ID: 13026

Tidal disruption events (TDEs), where a star is disrupted by a massive black hole provide a unique probe. They illuminate dynamics in galactic nuclei, and may provide constraints on rates of low frequency gravitational wave transients. A handful of candidates have been uncovered, with our recent discovery of a new class of relativistic TDE dramatically adding to the breadth of the population. Here we propose to characterise the spectral and temporal properties of of up to two TDEs found in AO11. As part of a multiwavelength campaign we will use XMM-Newton and HST to track the temperature; search for evidence of non-thermal components and study the long and short timescale variability. In doing so we will create unique panchromatic pictures of these events for the first time.

The Extreme X-Ray Weakness of PG 0043+039

Dr Norbert Schartel
XMM-Newton SOC, ESA
Program ID: 12952

The majority of broad absorption line quasars are X-ray weak which is usually explained by the absorption of the out-flowing wind in combination with the winds velocity shear. PG 0043-036 is the most extreme X-ray weak quasar known to date, but shows surprisingly only a very weak broad absorption line system. A conclusive interpretation is hampered by the absence of simultaneous measurements which is mandatory as both, the X-ray flux and the broad absorption system are known to be variable. We propose simultaneous XMM-Newton, HST (1 orbit) and 10m Hobby-Eberly or SALT Telescope observations in order to characterize simultaneously PG 0043-036’s X-ray emission and (broad) absorption (line system) properties.

Catching AGN in Deep Minimum States to Unveil Their Core Environment

Dr Norbert Schartel
XMM-Newton SOC, ESA
Program ID: 12953

The deep minimum state of AGNs is characterized by a strongly suppressed or even absent primary continuum. As the continuum disappears weak spectral features like relativistic iron lines or narrow soft X-ray emission lines from ionised plasmas become highly significant and their parameters can be determined. Therefore deep minimum states offer unique possibilities to investigate in detail the physics of the reprocessed components in AGN, including the immediate vicinity of the supermassive black hole. Applying our experience (several deep minimum observations) we propose two triggered 10ks XMM snapshot, one 80ks XMM follow-up and one HST (2 orbit) observation of an AGN in deep minimum state. We will identify deep minimum states based on Swift and XMM-Newton slew observations.

Physics of Black Hole Transients from Simultaneous X-Ray and UV Observations

Ms Alexandra Veledina
University of Oulu
Program ID: 12919

Fundamental questions concerning processes in the vicinity of black holes (BH) remain open. The accretion flow geometry, the role of the jet and the source of optical radiation are among most disputed. In recent years, simultaneous infrared/optical/ultraviolet--X-ray observations revealed their large potential in addressing these problems. By joining two powerful astrophysical techniques: (a) high-resolution X-ray spectroscopy and timing (which only XMM-Newton can provide) and (b) high time-resolution UV photometry (available only at HST), we will answer a number of fundamental questions of BH physics. We will constrain the accretion flow geometry, measure the inner disc radius, identify the source of seed photons for Comptonization, and locate the zone of the UV emission.

Testing the Paradigm of X-Ray Driven Exoplanet Evaporation with XMM+HST

Dr Peter Wheatly
University of Warwick
Program ID: 12920

HST observations show that two of the brightest transiting exoplanets are evaporating (HD209458b & HD189733b) and models suggest that the evolution of close-in planets may be dominated by this mass loss. It is believed that the evaporation is driven by X-ray irradiation of the planet by its parent star, but a lack of simultaneous measurements of irradiation and evaporation prevents a meaningful test of this model. We propose simultaneous XMM-Newton and HST observations of three transits of the brightest X-ray source, HD189733, in order to test the paradigm of X-ray driven evaporation and make a direct measurement of the efficiency of exoplanet evaporation.