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Hubble Space Telescope
XMM-Newton Joint Program Information

XMM-Newton Cycle 13/HST Cycle 22
Joint Program Overview

By agreement with the HST Project, the XMM-Newton Project may award up to 30 orbits of HST observing time each observing cycle. Similarly, the HST Project may award up to 150 ks of XMM-Newton time. The time will be awarded only for highly ranked proposals that require the use of both observatories and shall not apply to usage of archival data. The only criterion above and beyond the usual review criteria is that both sets of data are required to meet the primary science goals. Proposers should have taken special care in justifying both the scientific and technical reasons for requesting observing time on both missions. For these solicitations, no HST time will be allocated without the need for XMM-Newton time on the same target to complete the proposed investigation.

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.

IZw1 00 53 34.93 +12 41 36.19 COS/FUV G130M & G160M 8

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.

NGC 985 02 34 37.88 -08 47 17.02 COS/FUV G130M (2700s), G160M (3200s) and G140M (5400S) 5
NGC 985 02 34 37.88 -08 47 17.02 COS/FUV G130M (2700s), G160M (3200s) and G140M (5400S) 5

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.

L87326-X1 01 25 58.10 -01 17 14.80 ACS/SBC F115LP & F165LP 1
L87326-X1 01 25 58.10 -01 17 14.80 WFC3/UVIS F300W, F475W & F775W 1
L87326-X1 01 25 58.10 -01 17 14.80 WFC3/IR F125W & F160W 1

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

Dr. Anna Lia Longinotti
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.

Mrk 335 00 06 19.58 20 12 10.58 COS/FUV G140L (1300Å) 5
Mrk 335 00 06 19.58 20 12 10.58 COS/FUV G130M & G160M 2

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.

GSN 069 01 19 8.70 -34 11 30.50 STIS/FUV G140M 2
GSN 069 01 19 8.70 -34 11 30.50 STIS/NUV G230L 1

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.

CD-28-5104 07 55 52.85 -28 37 46.79 STIS/FUV E140M 1
CD-28-5104 07 55 52.85 -28 37 46.79 STIS/FUV E140M 1
CD-28-5104 07 55 52.85 -28 37 46.79 STIS/FUV E140M 1

The programs approved from the previous XMM Cycle 11 and Cycle 12 TACs can be found at the following links: