Prepared by: R. Mushotzky, NASA/GSFC, US Mission Scientist, the US XMM-Newton Users Group (R. Griffiths, Chair), and staff of the US RGS Team and the US XMM-Newton GOF
Copies of this document are available in: pdf and postscript formats.
On behalf of the US Newton X-ray Multi-Mirror Observatory (XMM-Newton) users community, the US Reflection Grating Spectrometer (RGS) Team, the NASA Goddard Space Flight Center (GSFC) Guest Observer Facility (GOF), and the NASA XMM-Newton Education and Public Outreach (E/PO) program, we request funding for the continued support of US participation in the European Space Agency (ESA) XMM-Newton mission. XMM-Newton's instruments provide unique data enabling US astronomers to continue to produce high-quality and significant results, at particularly low cost to NASA relative to other Great Observatory-class missions.
Continuing in the seventh Announcement of Opportunity (AO-7), the oversubscription by the world-wide community remains high, even increasing to a factor of 7.8 in time with 586 submitted proposals. The US astronomical community has been a major participant in the Guest Observer (GO) process throughout all AOs. In AO-7, 36% of the accepted proposals had US Principal Investigators (PIs), and an additional 33% had US Co-investigators (Co-Is). ESA has extended the XMM-Newton mission through at least 2012, and we anticipate a similar or better US response and success rate in future AOs. Moreover, with over 350 refereed papers per year (417 in 2006, at least 360 in 2007), with a commensurate proportion led by US authors, the scientific output from XMM-Newton remains high, and these results are cited four times more often than the average refereed paper in the astronomical literature.
The science goals and achievements of XMM-Newton are directly responsive to the 2006 NASA Strategic Plan1, providing important advances towards the strategic goal of ``Discovering the origin, structure, evolution, and destiny of the Universe, and search for Earth-like planets'' (Sub-goal 3D). XMM-Newton provides unique and necessary data for studies of the fundamental processes of neutron stars and black holes, the creation of the elements in supernovae and their dispersal in supernova remnants and starburst galaxies, the evolution of the elements on the largest scales in clusters and groups of galaxies, and the distribution of dark matter in clusters, groups, and elliptical galaxies. The study of active stars allows direct comparison with models of the early solar system and star forming regions for understanding the origin and evolution of stellar systems. XMM-Newton has examined relativistic processes from neutron stars and quasars, and constrained the spin of black holes in Active Galactic Nuclei (AGN). XMM-Newton also provides the capability of simultaneous X-ray and optical/ultraviolet (UV) observations. While the science areas of XMM-Newton, Chandra and Suzaku do overlap, each mission has been optimized differently in the six-dimensional space of angular resolution, bandpass, collecting area, spectral resolution, timing ability, and instrumental background.
The Senior Review panel has been asked to examine the question of ``Why are new data from older missions necessary?'' As shown below, XMM-Newton provides a broad range of exceptional data (from comets to quasars) to a large number of US GOs at low overall cost and has a rich scientific future.
There is no present mission, or any mission planned for launch
in the next five years which has XMM-Newton's combination of high
through-put X-ray imaging and spectroscopy and broad band
(optical and UV) capabilities. Constellation-X, the planned
successor to XMM-Newton
as well as Chandra, is more than a
decade away. The only other relevant mission is NeXT, a
Japanese-US mission which will have, if approved as a Small
Explorer Mission of Opportunity, a spectroscopic capability
superior to XMM-Newton's grating spectrometer but will not have
the angular resolution or collecting area of XMM-Newton.
As shown by the response of the US community to both the
Chandra and XMM-Newton AO's, these missions are
complementary, with XMM-Newton's wide field and high throughput
imaging and Chandra's unique high resolution
imaging capabilities. The grating spectrometers of the two
missions are also complementary as is Suzaku's broad band
(
keV) spectroscopic capability.
Because ESA and its member nations carry the brunt of the
costs for XMM-Newton operations, software development, and data
processing, the US community has access to ``Great Observatory''
science at a small fraction of the cost of the US operated
Great Observatories. The US community receives 
of the total XMM-Newton time and the mission is highly
productive. While removing the XMM-Newton funding would not,
legally, reduce the access of the US community to XMM-Newton's
new observations (AOs are open to the entire world), the
lack of funding for data analysis and interpretation and the
removal of GOF support would have a major impact on the
science productivity of the mission by reducing the
participation of the US community.
The future for XMM-Newton is bright with its unique properties for: 1) Science requiring many counts (but not necessarily high count rates) such as determining the abundance profiles of high-z clusters or the structure of AGN Fe K lines allowing the determination of black hole spin. 2) Science requiring long-looks or monitoring campaigns (i.e., variability studies) such as AGN timing or detailed studies of isolated neutron stars. 3) Science requiring multiwavelength observations using the XMM-Newton-unique Optical Monitor (OM), such as detailed studies of star forming regions. 4) Science using large samples of objects (legacy programs) utilizing the high ``speed'' of XMM-Newton observations such as studies of groups of galaxies. 5) Science using XMM-Newton's ability to obtain good signal-to-noise (S/N) spectra for weak sources such as the origin of the X-ray background and binary populations in nearby galaxies.
As new ground-based surveys such as the Sloan Digital Sky Survey (SDSS), the south pole telescope, and VISTA, as well as new space-based surveys from Spitzer and Herschel become available, XMM-Newton is the mission of choice for X-ray spectroscopic and timing follow-ups. In order to accommodate many of these capabilities the ESA project has modified the AO to introduce a new proposal type for very large programs allowing requests for 1-3 Ms of time and increasing the time dedicated to large and very large programs to about 30% of the total. To increase the usefulness of XMM-Newton for Targets of Opportunity (ToO) expected to come from GLAST and Swift, a new AO policy was introduced which allows the GOs to propose ToO observations of targets whose coordinates are not known at the time of submission (e.g., a new supernova)
Mission Overview
XMM-Newton is the second cornerstone of the ESA Horizon 2000 program. Launched on 1999 December 10, it remains in full operation and is in excellent health. ESA mission support is confirmed through 2012, with a possibility of future extensions. As of 2008 March, nearly 6500 targets have been scheduled for observation. All science data are made public after the expiration of a proprietary period, typically one year after data delivery. The XMM-Newton archive had 5600 observations publicly available as of 2008 March.
XMM-Newton observes in the 0.2-12 keV and optical/UV bands.
Its highly elliptical orbit allows long, uninterrupted
observations. This contiguous coverage (up to 
ks)
is more important now that Chandra is limited to
ks or less in many orientations.
The observatory has three co-aligned high throughput
7.5 m focal length X-ray telescopes with
full width at half maximum (FWHM)
angular resolution. The European Photon
Imaging Camera (EPIC) charge-coupled device (CCD) detectors
provide X-ray images over a 
field of view (FOV). Higher
resolution spectra (
)
are provided by the RGS that deflect half of the beam from
two of the X-ray telescopes, and these are the only high
spectral resolution instruments capable of observing extended
sources. The sixth instrument, the OM, is a
co-aligned 30 cm optical/UV telescope sensitive in the
1600-6500 Å band with a 
FOV and a wide variety of
modes. All the scientific instruments operate
simultaneously, providing exceptionally rich
data sets. The instruments can be run in a variety of
modes, allowing them to be tuned for the science needs
of a given observation.
XMM-Newton excels in providing high throughput X-ray imaging, timing, and spectroscopy for an extremely wide variety of astrophysical sources, from comets and planets to quasars and clusters of galaxies. With the EPIC and OM instruments constantly observing a large FOV, the well-calibrated and very large serendipitous source archive is a vast resource for ancillary research. However, only through the availability of XMM-Newton, Chandra, and Suzaku observations does the world community achieve the full complement of high angular resolution, high throughput, high spectral resolution, and low background in the 0.2-70 keV and optical/UV bands.
By the end of 2007 there were 1775 refereed papers published based on XMM-Newton data, with new papers appearing at the rate of one per day (see Figure 1 and the publication list2). Over the last two years XMM-Newton and Chandra have had similar numbers of refereed publications. The character of highly cited XMM-Newton papers is changing due to the publication of results from large XMM-Newton programs and combined analysis of XMM-Newton and other (e.g., Hubble, Chandra, Spitzer) data. We expect these trends to continue in the future and to amplify the impact of XMM-Newton results.
The XMM-Newton workshop on the future of the mission ``XMM-Newton: The
Next Decade'' held in 2007 June in Spain, identified a large
number of rich new science areas for XMM-Newton including studying
the intergalactic medium, the origin of ultraluminous galaxies,
the evolution of large scale structure, how AGN have
influenced the formation of structure,
detailed studies of nearby galaxies including their
interstellar medium, constraints on the equation of state of
neutron stars and the physics of star forming regions (to
mention a few). Some of this new science comes from the release
of the 
XMM-Newton serendipitous source catalog (2XMM) in
2007 October with 191,870 unique sources and the XMM-Newton Slew
Survey, released in 2007, which is 5 times more sensitive than
the best previous hard (2-8 keV) X-ray large solid angle survey.
These catalogs are a major resource for
archival research and provide a firm basis for future
observation proposals.
XMM-Newton's status as one of the world's pre-eminent astronomical
observatories is shown by the high proposal pressure,
publication rate, and the frequent citation
of refereed papers. In the last 3 years there have been more
than 65 XMM-Newton papers with more than 25 citations compared to
117 from Hubble. US scientists author of
the successful proposals and refereed papers, and would be placed
at a severe disadvantage in many areas of astrophysical research
without continued guest observer funding and support.
Given the health of the instruments and the satellite, the high oversubscription rate, the high fraction of the time going to US guest observers, the large archive and the rich scientific future we believe the continuation of the US XMM-Newton program at the present rate of funding is highly justified.
1 XMM-Newton Science
XMM-Newton's research program is peer-review driven with ToO possibilities, and thus it is very difficult to predict the next great discoveries. Every year since XMM-Newton was launched has seen major discoveries across many areas of science. One way of documenting the evolving scientific program is via the accepted large projects. Starting in AO-3 these have included surveys of clusters of galaxies across a wide range of redshifts, monitoring of the galactic center, a large solid angle deep X-ray survey, and a survey of the Taurus molecular cloud. AO-4 brought projects to study the intergalactic medium, timing observations of ultra-luminous X-ray sources, time variability of AGN Fe lines, and the spin rate of an isolated neutron star. In AO-5 there were a deep and wide survey of M31, a follow-up of Swift BAT sources, a very large but relatively shallow X-ray survey to search for large scale structure, measuring the ionization structure of ``dipping'' X-ray binaries, and a study of the relativistic double pulsar PSR J0737-3039. AO-6 had an investigation of the outer regions of a galaxy cluster, a study of Orion's population of young stars, deep grating observations of low redshift clusters, and a RGS study of shell-type supernova remnants with X-ray synchrotron radiation. AO-7 large projects include a survey of nearby stars with planets, X-ray timing studies of X-ray pulsars, mass profiles of galaxy clusters, and a survey of the SN 1006 supernova remnant. There have been over 25 press releases on XMM-Newton science in the last two years.
The next dedicated XMM-Newton Symposium, ``The X-ray Universe 2008'' to be held in Granada, Spain, is expected to be well-attended (the last such meeting had over 320 participants) with many new results. XMM-Newton is also well represented at a wide variety of international and national astronomical meetings.
The future science of XMM-Newton is considerably enhanced by the availability of the 2XMM, Slew Survey, and OM catalogs, which provide ``finding charts'' for future proposals and large samples of all types of objects. These databases enable not only direct archival research but also new GO programs. The phase space for discovery with XMM-Newton has increased through the years. For example, continual improvements in calibration and the advent of new software allow diffuse background studies and measurement of the mass profiles of clusters, measurements of the soft X-ray background and the galactic plane emission. The continued development of the basic Science Analysis System (SAS) has made analysis easier and more robust as well as providing new automatic data products, easing the analysis of the large and complex data sets. We believe that the best is yet to come from XMM-Newton.
The wealth of XMM-Newton results requires a focus on a small fraction
of the representative results. With more than 1350 accepted
GO proposals and 
refereed papers, more than 750 in
the last two years, the following is just a taste of what has
been accomplished in the last two years, and suggests what
the future might hold.
1.1 Active Galactic Nuclei (AGN)
XMM-Newton observations of AGN continue to provide the highest quality
spectral and timing data, crucial for understanding the origin of
the continuum and the nature and
distribution of matter near the black hole. The innermost
regions of AGN where the bulk of the energy is produced can be
investigated only by sensitive X-ray
observations. The intensity and the profile of the iron emission
lines near 6.4 keV provide a unique diagnostic tool to understand
accretion processes in the vicinity of the black hole where the
effects of
strong gravity (e.g., gravitational redshift and light bending in
curved space-time) are important. One of the most recent
highlights is that systematic studies of large (
) samples of
AGN demonstrate that most of the ``well-exposed'' objects (i.e.,
with 
counts) do indeed show broad Fe K profiles
(Figure 2; Guainazzi et al. 2006;
Nandra et al. 2007) indicating the importance of relativistic
processes. Moreover
there are a significant number of sources showing transient and/or
modulated variations of the Fe K line (see e.g., Tombesi et al. 2007;
Petrucci et al. 2007). Such observations offer the opportunity to
directly estimate the black hole mass and spin (a), and test theoretical
models describing the innermost regions of accretion disks around
AGNs. Brenneman &
Reynolds (2007), in the first ever survey of black hole spin, analyzed
a set of high S/N XMM-Newton AGN spectra placing robust
constraints on black hole spin from moderate (a
0:5-0:7) to high
(a
0:85). The validity of such observations have been supported by
detailed comparisons of Suzaku and XMM-Newton observations of several
AGN (Reeves et al. 2007) which have shown that both sets of data are
virtually identical, confirming that the EPIC and the Suzaku
XIS are extremely well cross calibrated.
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The XMM-Newton high count rate for AGN studies combined with
long and uninterrupted observations has allowed a
direct comparison of properties of Galactic and extragalactic black
holes. Summons et al. (2007) and Arévalo et al. (2006) have shown
that the timing properties of AGN can be
well modeled by the same
processes seen in Galactic black holes making
a fundamental connection between black holes across a mass range of
in mass. XMM-Newton's unique properties
have allowed the detections of lags and leads between different
spectral bands (McHardy et al. 2007) giving unique insight into the
physical mechanisms producing the X-ray photons.
The high S/N of XMM-Newton RGS spectra from a long observation of NGC4051 (Krongold et al. 2007) was used to determine the total power in an AGN's wind for the first time, and thus provided the first constraints on the ability of AGN to control the formation of structure in the Universe. XMM-Newton observations of the cavities produced in clusters by radio sources (Gitti et al. 2007) have revealed the enormous power in relativistic AGN winds, while an XMM-Newton follow-up of hard X-ray selected sources from Integral and Swift (Winter et al. 2008) has shown a wide variety of X-ray spectral types which have challenged the unified model of AGN and models for the origin of the X-ray background. The availability of the XMM-Newton archive has made available the first large sample of the average high resolution spectra of AGN (Kaastra 2008) revealing a wealth of previously unknown spectral features.
Future AGN research: This will concentrate on high S/N Fe K line studies to determine black hole spin and the origin of variable Fe K lines, detailed follow-up studies of ``new'' highly obscured AGN discovered by Spitzer, Swift BAT, SDSS, and Integral, and deep exposures of a sizable sample with the RGS to understand the energetics of AGN outflows and the possible existence of broad low energy lines. Reverberation studies will require three or four well-sampled sources, each with about 1 Ms exposure, showing the size of potential programs.
1.2 Clusters of Galaxies and Dark Matter
The intracluster medium (ICM) in clusters of galaxies comprises
most of the baryons in the cluster. XMM-Newton's large collecting
area, good spatial resolution and large FOV (
radius), and
a better high-resolution spectrometer
for extended sources than Chandra make it the premier instrument
for cluster spectroscopy.
Recent XMM-Newton results have shed new light on the complex physics that
governs the evolution of the baryonic components in clusters.
Zhang et al. (2007) established that the gas
entropy exceeds the value attainable through gravitational heating
not only in the core but throughout the whole ICM. This is direct
evidence that physics other than gravity has had a major impact of
the formation of groups and clusters and is key to the understanding
of the effects of feedback on the formation of structure. Studies
of distant clusters are measuring the size of the feedback through
cosmic time. Two recent XMM-Newton
studies of distant clusters, surprisingly show no significant
departure from the evolution expected in the standard self-similar
model up to 
which assumes, incorrectly, that all the entropy
comes from gravitational physics.
One of the most surprising recent XMM-Newton cluster discoveries
was that of a candidate ``fossil cluster'' (Gastaldello et al.
2007) at 
. It has normal X-ray properties with a
temperature of 3.6 keV and bolometric luminosity of
erg s
- but only one very bright
elliptical galaxy. This object
is thought to be the long-term dead end of gravitational evolution
where the central galaxy has assimilated
the stellar content of the
member galaxies into a huge extended halo.
Given
that in most systems there is a strong relationship between the galaxy
content and the cluster mass this result was quite unanticipated. The
best interpretation is that this system was formed at very high redshift
and thus is a ``true'' fossil of the Universe.
The evolution of clusters can
provide crucial information about the nature of the ``dark energy.''
But in order for cluster cosmology to achieve its promise, an improvement
in the understanding of cluster physics is needed; understanding the
relationship between a cluster's mass and its X-ray luminosity, its
temperature, and its gas mass. Significant progress was made in this area
including the first
precise calibration of the mass-temperature relation in the local
Universe (Croston et al. 2008). Studies of these
crucial scaling relations are just now beginning with the
availability of large samples over an interesting range of
redshifts and X-ray luminosities. Early results show that
the cluster masses and gas mass fractions measured for an
unbiased, flux-limited and nearly volume-complete sample
of 13 clusters
at 
and Zhang et al. (2006) are consistent with
self-similar behavior for
the gas fractions at radii larger than
.
A major breakthrough in the understanding of the XMM-Newton EPIC detector background allowed Snowden et al. (2008) to derive robust temperature, density and abundance profiles and maps for large clusters providing the data for detailed comparison with cluster models.
Galaxy Formation and X-ray Cluster Science:
Observations of metal and entropy distributions constrain the
two most prominent processes in galaxy formation: star formation
and AGN formation. Tozzi
(2008) measured the distribution and level of iron enrichment
to
Gyr and claimed a factor of two
evolution in the Fe abundance consistent with a burst from massive
ellipticals at 
and slower enrichment from disks later on.
 |
A study of M87 (Forman et al. 2007) revealed that shocks may be the most significant channel for AGN energy input into cluster cooling cores. A violent outburst of the central AGN may also play a fundamental role in shaping the global properties of clusters as seen in MS 0735+7421 (Gitti et al. 2007).
Considerable progress was made in understanding the effects of
relativistic particles in providing pressure and heating the gas. The
combination of radio and X-ray observations provides a measure of the
magnetic field independent of equipartition or minimum energy assumptions.
Chen et al. (2008) found that XMM-Newton data give a lower limit to the
magnetic field which is larger than equipartition.
Belsole et al. (2007) showed that 60% of powerful radio galaxies in the
redshift range from 
lie in a luminous X-ray cluster, and all but
one narrow-line radio galaxy are in a cluster environment. Therefore there
is no strong evidence that the presence of a radio source requires a
peculiar environment.
The unique power of RGS spectroscopy of extended sources was
demonstrated by Sanders et al. (2007) who detected strong
N VII emission, indicating supersolar N abundance in the
central regions of clusters, a strong constraint on the
nature of the stars that have produced the metals. They also
showed that the lack of RGS detections of cool gas in other
clusters could be due to their relatively short, 
ks,
exposures, indicating that
longer XMM-Newton exposures, possible with the new large programs,
will strongly constrain the emission measure distribution of
the cooling gas in clusters.
Future of cluster research: A major step forward in our
understanding of dark matter structure formation and dark energy
is expected by combining XMM-Newton surveys, e.g., the XMM Cluster
Survey (XCS; Pierre et
al. 2007) with more than 2000 cluster candidates, more than 300
with measured redshift including the most distant cluster ever
known at 
, and the forthcoming Planck data. The
Planck whole sky survey will increase by two orders of
magnitude the number of known very massive (
keV) clusters
at 
, the best objects for precise cosmology with clusters.
XMM-Newton follow-up will be crucial to fully exploit this sample,
allowing constraints on the dark energy equation of state from
the gas mass fraction (used as standard candle) and from cluster
abundance (which requires a precise calibration of the mass
Sunyaev-Zeldovich observable relation). In addition, these
observations will
allow a full test of dark matter collapse models from detailed
studies of the mass profiles and their evolution with redshift.
1.3 Diffuse X-ray Emission in Galaxies
XMM-Newton observations of edge-on early-type disk galaxies have confirmed
the detection of hot gas in extended halos. The diffuse X-ray emission
from the edge-on Sa galaxy M104 (Sombrero) has two components, one
distributed like the stellar K-band light (due primarily to residual
emission from discrete sources), and diffuse hot gas extending to
20 kpc from the galactic center with 
keV
(Li et al. 2007). However, in NGC 2613 the diffuse emission
is distributed in discrete bubble-like features extending from
the disk out into the halo (Li et al. 2006), unlike the smooth
hot gas halo of M104. In NGC 6810 the extraplanar diffuse X-ray
emission is spatially associated with diffuse H
emission
and H filaments, suggesting the presence of a ``disk-wide''
superwind (Strickland 2007).
XMM-Newton observations of the X-ray-bright elliptical galaxy NGC 4649 detected ``fingers'' similar to radial features seen in hydrodynamic simulations of cooling flows in elliptical galaxies, and might be due to convective motions of hot outflowing gas and cooler inflowing gas (Randall et al. 2006). Recent results on NGC7619 in the Pegasus group shows the first clear pictorial evidence of the process of metal enrichment of the ICM as a result of galaxy-cluster dynamical interaction (Kim et al. 2007). In M87, Simionescu et al. (2007) have, for the first time, found evidence that cold, metal-rich gas is being transported outwards, possibly through bubble-induced mixing as the radio lobes rise along the short axis of the elliptical pressure distribution, following the steepest gradient of the gravitational potential, and contain a nonthermal pressure component. In a parallel result, deep RGS observations of M87 (Werner et al. 2006) determined, for the first time, accurate abundance values for C and N in the hot gas. The comparison of the abundance ratios of C, N, O, and Fe in the intersellar medium (ISM) of M 87 with those in the stellar population of our Galaxy shows that the relative contribution of core-collapse supernovae to the enrichment of the ISM in M 87 is significantly less than in the Milky Way, and indicates that the enrichment of the ISM by Fe through Type Ia supernovae and by C and N is occurring in parallel.
1.3.1 Diffuse Hot Gas in the Milky Way
Recent X-ray observations of distant quasars have detected
O VII absorption at near-zero redshift, which could originate
from a hot gas halo of the Galaxy or the ICM in the Local Group.
Archival XMM-Newton RGS observations of 25 AGNs and LMC X-3 were
analyzed to measure the O VII K absorption line strength.
The data are in conflict with a purely Local Group model but
support the Galactic halo model since the O VII absorption
equivalent width is well correlated with the Röntgensatellit
(ROSAT)
measurements of the background emission in the R45 band
(0.4-1 keV), for which O VII emission makes the largest
single contribution (Bregman & Lloyd-Davies 2007; Fang et
al. 2006). These observations prove that the Milky Way has a
moderate scale height hot gas halo whose mass is considerably
less than that predicted by cold dark matter (CDM) models
Archival XMM-Newton observations of 11 galaxy clusters have been
used to measure the oxygen abundance of the Milky Way's ISM
by analyzing the K-shell X-ray photoionization edge in the
X-ray spectra (Baumgartner & Mushotzky 2006). It is found
that at high Galactic columns above 
cm
the X-ray columns are generally 1.5-3.0 times
greater than the 21-cm H I columns, indicating that molecular clouds
become an important contributor to 
and that the average
ISM O abundance (O/H) is
(4.85
0.06)
10
, or 0.99 solar when using the most
recent solar photospheric values. Since X-ray observations are
sensitive to the total amount of oxygen present (gas+dust), these
results indicate a high gas-to-dust ratio. Also, the oxygen
abundances along lines of sight through high Galactic columns
are the same as abundances through low columns, suggesting that
the composition of denser clouds is similar to that of the more
diffuse ISM.
The X-ray spectrum of the Local Bubble was studied by
analyzing spectra from two XMM-Newton pointings on and off an
absorbing filament in the southern Galactic hemisphere
(Henley et al. 2007). This Local
Bubble emission is consistent with that from a plasma in
collisional ionization equilibrium with a temperature
and an emission measure
of 0.018 cm
pc. This temperature is in good agreement
with that derived from the ROSAT All-Sky Survey.
Future Programs: Studies of the diffuse X-ray emission from the disk, bulge, and nucleus of the Milky Way and other nearby normal galaxies will be considerably enhanced by the new background subtraction software allowing the statistical limits of the data to be reached. This will allow analysis of the vast archive of ``effective'' ISM pointings for a detailed map of the diffuse emission in the Milky Way.
1.4 Supernova Remnants and Neutron Stars
1.4.1 Supernova Remnants (SNR)
Supernovae (SNe) produce the heavy elements and SNR distribute these elements throughout the ISM and disturb and compress the material in the ISM producing the conditions which are necessary to form the next generation of stars. As extended objects with high temperatures and a complex set of abundances and ionization conditions, SNRs are prime objects for study with XMM-Newton providing rich spectra on physically important spatial scales. Spatially resolved SNR spectra separate thermal from non-thermal emission, identify stratification of ejecta, separate the forward and reverse shock regions, measure variations in temperature and ionization conditions.
The extraordinarily high quality of the XMM-Newton EPIC spectral data
have provided the relative ratios of the elements Si, S, Ar, Ca, Cr,
Mn and Fe in several remnants which, for the first time, can test
detailed explosion models for Type Ia SNe (Badenes et al. 2006;
Kosenko 2006). Another example of XMM-Newton's spectral capabilities
is SNR W49B (Figure 4) for which Miceli et al.
(2006) concluded that the abundances are not consistent with a
-ray burst progenitor.
XMM-Newton spectra of the LMC SNRs DEM L238 and L249 detected
a surprisingly large abundance of Fe at high ionization timescales
interior to the remnant (Borkowski et al. 2006). Such a large amount
of Fe near to ionization equilibrium is at odds with models of Type Ia
SNe and may indicate that there is new class of these explosions.
XMM-Newton data from clusters were used by de Plaa et al. (2007)
to derive average nucleosynthetic yields from Type Ia
SNe which favor the delayed detonation models.
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SNRs are thought to be primarily responsible
for the acceleration of cosmic-rays up to energies of
GeV. The observational evidence for this
phenomenon has only been acquired recently and XMM-Newton has
contributed significantly to these discoveries via detailed
measurements of particle spectra and the magnetic fields.
Vink & Kuiper (2006) separated thermal and non-thermal
emission in the galactic SNR RCW 86 using XMM-Newton spectral
and imaging capabilities (Figure 5).
Analysis of
the non-thermal emission indicated a magnetic field of
and a shock velocity of
km s supporting the association of
RCW 86 with SN 185. Importantly, the broad band high S/N
XMM-Newton spectrum reveals that a simple power-law cosmic-ray
electron spectrum with an exponential cutoff cannot
explain the broadband synchrotron emission. Instead, a
concave electron spectrum is needed, as predicted by
nonlinear shock acceleration models.
The shape and spectra of pulsar wind nebulae (PWNe)
depend on the angular distribution, magnetization, and
energy spectrum of the wind streaming from the pulsar
magnetosphere, as well as on the pulsar velocity and the
properties of the ambient medium. XMM-Newton observations have
detected new PWN in G337.2+0.1, DEM L241, and around PSR
B0355+54. The PWN in G328.4+0.2 has been studied in detail
by Gelfand et al. (2007) who conclude that the X-ray
emission is consistent with a 
yr old PWNe
formed by a low magnetic field (
G) neutron star,
spinning rapidly (
10 ms), in an undetected SNR with a
high explosion energy (
ergs) and a relatively
low amount of ejecta (
).
Future Prospects: Thanks to its high sensitivity, reasonable angular resolution, and large field of view, there are a large number of projects to be carried out on SNRs. These include the study of nucleosynthesis products in nearby or middle-aged SNRs and shock physics using deep RGS observations of specific remnants or regions. The study of electron acceleration using deep spatially resolved spectroscopy in extended SNRs (e.g., SN 1006, G347.3-0.5, Vela Junior) can be used to search for the maximum energy of accelerated particles, azimuthal variations in particle acceleration, and to determine the density of the thermal plasma. The followup of High Energy Stereoscopic System (HESS), Integral, and GLAST sources with XMM-Newton will constrain proton acceleration from a detailed comparison of the X-ray and the TeV emission.
1.4.2 Neutron Stars (NS)
XMM-Newton observations of the ``bursting'' behavior of the Anomalous X-ray Pulsars (AXPs) have been essential in characterizing the complicated processes by which a NS relaxes after the burst. In AXP 1E 2259+586 (Zhu et al. 2008) and AXP 4U 0142+61 (Gonzalez et al. 2008) the flux and hardness ratio are correlated (both increasing) after the burst, and this behavior can be explained by both the ``twisted magnetosphere'' model of Thompson et al. (2002) and the surface thermal emission model of Özel & Güver (2007). Phase-resolved spectroscopy with high statistical precision data (Rea et al. 2007) show significant variations with phase but none of the spectral features expected from an atmosphere of a highly-magnetized NS. The detection in the isolated NS RX J1856-3754 of a 7 s period by Tiengo & Mereghetti (2007) at the extremely low level of only 1.2% modulation, is a testament to the sensitivity of XMM-Newton observations and confirms that RX J1856-3754 belongs in the class of the nearby, thermally-emitting NS with soft X-ray spectra. Continued XMM-Newton observations of another member of this class, RX J07204-3125, which does show broad spectral features which vary significantly in time (Haberl et al. 2006a), suggest that the time-variable spectral features can be explained by the precession of the NS if there are two hotspots which rotate into view at different times. In each of these cases, repeated observations of the same source with XMM-Newton was the key to making the discovery.
XMM-Newton detected a 6.67 hr period of 1E 161348-5055 at the center of SNR RCW103 which has an age of 2000 years (De Luca et al. 2007). This period is much too long for a 2000 year old star, which should be rotating thousands of times faster. This could be the first example of a low-mass X-ray binary (LMXB) associated with a SNR, and thus the first LMXB for which we know the precise birth date, just 2000 years ago. Alternatively, if it is an isolated NS, the unprecedented combination of age, period and variability may only fit in a very unusual scenario, featuring a peculiar magnetar, dramatically slowed-down over 2000 years, possibly by a supernova debris disc.
XMM-Newton has provided new evidence that some pulsars are born
spinning relatively slowly with relatively low values of the
magnetic field. Gotthelf & Halpern (2005) placed an upper limit
on the period derivative of 1E 1207-5209 suggesting a magnetic
field of
and a characteristic age
of 27 Myr assuming a dipole spin-down, inconsistent with the
age of the remnant and suggesting the pulsar was born spinning
close to its current period of 424 ms. Mori &
Hailey (2006) have shown that the spectral features in
1E 1207-5209 can be explained by an atmosphere which contains
O and Ne and has a characteristic magnetic field of
. Another NS which shows
evidence for a weak magnetic field and a slow, stable rotation
is J1852+40 in the SNR Kes 79. Halpern et al. (2007)
use a similar technique to estimate a magnetic field strength
of
and a characteristic age of
8 Myr, which is again wildly inconsistent with the age of the
remnant. They suggest that this might point to a scenario for
the formation of radio-quite Compact Central Objects (CCOs).
The key to these discoveries was again repeated observations of the
same source with the high sensitivity of XMM-Newton. The coming
years promise more such discoveries as XMM-Newton will be able to
make repeated observations of more sources.
For the milli-sec pulsars PSRs J0030+0451 and J2124-3358
(Bogdanov et al. 2007) the relatively large pulsed
fractions observed require the existence of a light-element
atmosphere and cannot be reproduced
by a blackbody model for realistic NS radii. Modeling of
their spectra placed constraints on their compactness of
km and 
km (68% confidence) assuming
M. or more generally
and
, a major constraint on the equation of state of NSs.
Future Prospects: AGILE and GLAST will certainly discover more Geminga-like NSs and Integral will find new candidate neutron stars. Deep observations of black hole sources in quiescence will constrain the physics of advection-dominated accretion flow (ADAF) models and high S/N observations of quiescent systems will allow the determination of the inclination of the system from the X-ray light curve.
1.4.3 X-Ray Sources in Other Galaxies
The deep XMM-Newton survey of M31 is a major milestone allowing the detailed study of the source populations and individual sources (Stiele et al. 2007, 2008; Figure 6). This survey revolutionized our study of extragalactic X-ray binaries providing data of the quality that were previously only possible for X-ray binaries in the Milky Way and the Magellanic Clouds. Stiele et al. (2008) have matched supersoft sources discovered in the XMM-Newton survey with optical novae observed in M31 . TheXMM-Newton spectra of an X-ray transient suggests that it is a black-hole X-ray nova. Two of the supersoft sources are periodic (at 865 s and 217 s; Osborne et al. 2001; Trudolyubov & Priedhorsky 2008) suggesting that they are rotating, magnetic white dwarfs.
 |
Trudolyubov et al. (2007) have discovered a transient
accreting X-ray pulsar in NGC 2403. This remarkable
system shows an extremely high luminosity during its outburst
of
erg s, 10 the Eddington
limit for a neutron star and a very fast decrease in its
pulsation period during the outburst. Its X-ray luminosity
is high enough to account for the observed spin-up rate,
assuming that the X-ray source is powered by disk
accretion onto a highly magnetized neutron star. Optical
follow-up (Zepf et al. 2007) of a luminous time variable
XMM-Newton source in the elliptical
NGC4472 showed [O III] emission, sealing the case for
it being a black hole in
a globular cluster, the first ever found.
1.4.4 Ultraluminous X-Ray Sources (ULXs)
These sources have an X-ray luminosity,
erg s, which exceeds the Eddington limit of
black holes with masses of order 15 M
, and are
suspected to either have ``super-stellar'' mass black holes
or to beam their emission towards us. Only XMM-Newton can deliver
light curves and spectra with the very high S/N needed to
find indirect indicators
of the mass, such as breaks and quasiperiodic oscillations
(QPOs) in their X-ray power spectra. These observations
have led to the identification of QPOs in several ULXs
(e.g., Strohmayer et al. 2007; Dewagan et al. 2006) as
well as measurements of the slope of their low-frequency
power spectra suggesting that the masses of the compact
objects in these ULXs are of the order of 100 M
or greater, consistent with a new type of object.
The high-S/N XMM-Newton spectra allowed Winter et al. (2007)
to probe their immediate gaseous environments by measuring
the oxygen (and sometimes the iron) abundance in the host
galaxy. They found that the abundances are similar in all
ULXs and comparable to the abundances of H II regions,
despite the fact that their host galaxies have very diverse
properties. Moreover the column density along the line of
sight can be attributed to the intervening interstellar
medium.
1.4.5 Cataclysmic Variables (CVs) and Related Objects
In a recent paper
Ramsay et al. (2006a) present sensitive observations of
a system with one of the shortest orbital periods,
RX J1914+24, determining that the orbit is decaying at a
rate of
s s consistent with the
emission of gravitational waves from this system. In a
separate study of the X-ray properties of a sample of seven
AM CVn stars Ramsay et al. (2006b) discovered a strong
anti-correlation between the UV luminosity, measured
by the OM, and the orbital period, which provides a strong
test of models for the accretion process in these systems.
Using the XMM-Newton X-ray spectra, these authors discovered a
strong overabundance of N, a test of the evolutionary
processes that led to their formation.
1.5 Stars
1.5.1 X-ray emission from Pre-Main-Sequence Stars
The XMM-Newton Extended Survey of the
Taurus molecular cloud (XEST) (Güdel 2008 and 14 papers
in a special feature of 2007, A&A, 468) significantly
improved the sampling of X-ray emission from young stars in the
Taurus-Auriga star formation region (SFR). It is the closest
and best-studied large SFR and has served
as a test-bed for low-mass star formation theory for decades.
XMM-Newton provided unprecedented spectroscopic results from
nearly every observed T Tauri star, and from 
% of the
studied brown dwarfs and protostars. The survey includes the
first coherent statistical sample of high-resolution spectra
of T Tauri stars, and is accompanied by a U-band/UV
imaging photometric survey with the OM. XEST led to the discovery
of new, systematic X-ray features, not possible before with
smaller samples and lower S/N, in particular the X-ray soft
excess in classical T Tauri stars indicative of accretion
and the two-absorber X-ray
spectra of jet-driving T Tauri stars. In an on-going
program, Wolk et al. (2008) surveyed the X-ray emission from young
stars in Orion (Figure 7) over a far greater
spatial area than covered by the Chandra COUP observations.
 |
The wide field imaging of the EPIC cameras provides efficient X-ray sampling of young stellar clusters, with the RGS providing grating spectra for studies of the coronal temperature and density distributions.
Accretion-induced X-ray emission is
indicated by high electron densities,
unusual patterns of elemental abundances, and low temperatures. The
XEST survey confirms that the soft
excess is certainly confined to accreting stars, the
densities in the plasma are often too low for the X-rays to originate
in the accretion shock itself (Telleschi et al. 2007abc; Güdel et al.
2007), and that the accreting material produces an excess of
cool 1 MK plasma, rather than suppressing the coronal heating process
that produces the typical 
K hot plasma (Güdel & Telleschi 2007).
Stelzer et al. (2006) detected a dramatic (30 increase
in X-ray count rate and 6 magnitudes at V using the OM) flare
on the older (300 Myr), ultracool M8 dwarf LP 412-31. This flare
showed physical evolution compatible with
a single impulsive injection of
ergs
of energy into the corona of
this very low mass star over a 4 minute time interval, which was then
reradiated as X-rays for the next 30 minutes.
1.5.2 High Mass OB and Wolf-Rayet Stars
Changes in the X-ray luminosity, temperature, and absorption
in colliding wind binaries (CWB) allow the wind
properties of both components of the systems to be investigated.
Skinner et al. (2007) used spectral fits with a
constant-temperature plane-parallel shock model to derive a shock
temperature
keV (
MK),
hotter than can be accounted for
using 2D numerical colliding wind shock models based on nominal
mass-loss parameters. Hamaguchi et al. (2007) observed 
Car
through its 2003 X-ray minimum and found a large (
)
increase in the hydrogen absorption column towards the star. These
variations were qualitatively consistent with emission from the
wind-wind collision plasma entering into the dense wind of the
massive primary star. They also discovered an additional X-ray
component that exhibited no variation on timescales of weeks to
years which is probably produced by the collision of high-speed outflows at
km s from Car with ambient gas
within a few thousand AU from the star. Phase-dependent X-ray
variability was also found for a similar star, the massive SMC
binary HD5980 (Nazé et al. 2007).
The X-ray emission from single O stars is thought to arise
from shocks within the massive winds and emission generated
in magnetic structures. The observation of N VI and C VI
resonance lines in RGS spectra (Leutenberger et al. 2007)
allowed the examination of evidence for resonance
scattering which can alter the He-like triplet resonance line
profiles. Inclusion of this effect in spectral
fitting has the potential to reduce discrepancies between the
mass loss rates derived from UV and X-ray data.
Pollock (2007) used XMM-Newton spectra of 
Ori to study
the role of collisionless shocks far out in the wind as the
source of the observed X-ray emission; such shocks would be
magnetically controlled and should behave significantly
differently than cooling shocks in the wind acceleration region.
Future: XMM-Newton has the capability of providing high S/N grating spectra for moderate-sized samples of many types of stars, drastically increasing the present sample size. In addition, detailed studies of the hosts of planets will provide information of the X-ray radiation fields around these stars that will allow far more refined simulation of the high energy processes affecting the atmospheres of these planets. Surprisingly, out of over one hundred stars (as of early 2007) known to harbor extrasolar planets, about 35 are known to emit X-rays and studies of volume limited samples of field stars yield detection rates approaching 100%. XMM-Newton is ideally suited to study the X-ray emission of very young open clusters containing a large number of O-type stars (e.g., NGC6231; Sana et al. 2006) and there are at least eight more clusters that are rich in O-type stars and have not yet been observed with XMM-Newton or Chandra.
24pt1.6 Cosmology, Surveys, Serendipitous Science
The XMM-Newton serendipitous data provide a deep, large area sky
survey with an extended energy range, allowing detection of
large numbers of obscured and
hard-spectrum objects absent in earlier surveys.
The survey catalog, 2XMM, was released in 2007
August and is the largest catalog of X-ray sources containing
detections of 
unique
sources drawn from 3491 public XMM-Newton observations covering
more than 500 deg
. The catalog is accompanied by X-ray
spectra and time series for the brighter sources (amounting
to 
% of the total); these associated
data products are a major resource in their own right.
This catalog complements deeper Chandra and XMM-Newton small-area surveys, probing a large sky area at the flux limit corresponding to the objects that contribute to bulk of X-ray background. It provides a rich resource for generating large, well-defined samples since X-ray selection is a highly efficient technique for selecting AGN, clusters of galaxies, interacting compact binaries, and active stellar coronae. As an example, Page et al. (2007) have explored the properties of the harder sources, finding that their average spectra are harder than that of the X-ray background, and that they are absorbed AGN.
The ESA XMM-Newton project has developed a Slew Survey
(Saxton et al. 2008) in which the X-ray data are
recorded while the spacecraft slews across the sky from
one target to another. This has produced the best ever hard band
(2-8 keV) X-ray survey with 
sources deg.
One of the more spectacular results
from this survey has been the discovery of two new candidate
giant amplitude X-ray flares which are thought to be due to the
tidal disruption of a star by a quiescent supermassive black
hole at the center of the galaxy (Esquej et al. 2007).
The survey has, so far, 4700 relatively bright X-ray sources
with positions better than 
over 14% of the sky
(Saxton et al. 2008). The slew survey should cover most of
the sky over the next few years and is a great source of rare,
X-ray bright objects suitable for further study. The XMM-Newton GOF
(Kuntz et al. 2008) has produced the OM source catalog with
over 
sources in 3 UV filters and 3 optical
filters in 4950 fields producing optical counterparts for
many of the 2nd XMM source catalog. This catalog is also a
good resource for comparison with SDSS and GALEX data.
 |
COSMOS Survey: XMM-Newton surveyed the COSMOS HST
2 deg field (Figure 8), the largest
survey undertaken with HST. This combined with ground-based
redshifts from the VLT has resulted in the first 3-dimensional
map of dark matter across the COSMOS field and extending
back in time by about six billion years. The 3-D X-ray map
has shown that normal matter, as evidenced by X-ray emitting
clusters of galaxies, accumulates along the densest
concentrations of dark matter which are shown by weak
gravitational lensing.
Future: Results from the approved large program on a wide angle survey will soon be forthcoming as will the results on a deep observation of the Chandra deep field south approved in AO-7. The workshop on ``An XXL Extragalactic Survey: Prospects for the XMM Next Decade'' will be held 2008 April 14-16 in Paris France and will consider a wide variety of future options for XMM-Newton surveys.
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Appendix 2: List of Acronyms
| 2dF | Two Degree Galaxy and Quasar Survey |
| AAVSO | American Association of Variable Star Observers |
| AAS | American Astronomical Society |
| ACS | Advanced Camera for Surveys |
| ADP | Astrophysics Data Program |
| AGN | Active Galactic Nuclei |
| AO | Announcement of Opportunity |
| ASCA | Advanced Satellite for Cosmology and Astrophysics |
| AXP | Anomalous X-ray Pulsar |
| BAL | Broad Absorption Line |
| BAT | Burst Alert Telescope |
| CCD | Charge-Coupled Device |
| CCF | Current Calibration Files |
| CCO | Compact Central Object |
| CDM | Cold Dark Matter |
| CLEA | Contemporary Laboratory Experiences in Astronomy |
| CMU | Carnegie Mellon University |
| Co-I | Co-Investigator |
| CSM | Circumstellar Matter |
| CTI | Charge Transfer Inefficiency |
| CU | Columbia University |
| CV | Cataclysmic Variable |
| CWB | Colliding Wind Binaries |
| DPU | Digital Processing Unit |
| EA | Educator Ambassadors |
| EPIC | European Photon Imaging Camera |
| E/PO | Education and Public Outreach |
| ESA | European Space Agency |
| ESOC | European Space Operations Center |
| FOV | Field of View |
| FTE | Full Time Equivalent |
| FWHM | Full Width at Half Maximum |
| FY | Fiscal Year |
| GALEX | Galaxy Evolution Explorer |
| GBH | Galactic Black Hole |
| GLAST | Gamma-ray Large Area Space Telescope |
| GO | Guest Observer |
| GOF | NASA/GSFC Guest Observer Facility |
| GPG | Public domain version of Pretty Good Privacy |
| GRB | Gamma-Ray Burst |
| GSFC | Goddard Space Flight Center |
| GT | Guaranteed Time |
| GTN | Global Telescope Network |
| HEASARC | High Energy Astrophysics Science Archive Research Center |
| HESS | High Energy Stereoscopic System |
| HETG | High Energy Transmission Grating |
| HPD | Half Power Diameter |
| HST | Hubble Space Telescope |
| ICM | Intracluster Medium |
| IGM | Intergalactic Medium |
| INS | Isolated Neutron Stars |
| INTEGRAL | International Gamma-Ray Astrophysics Laboratory |
| IR | Infra Red |
| IRAS | Infra Red Astronomical Satellite |
| ISM | Interstellar Medium |
| ITEA | International Technology Education Association |
| JPL | Jet Propulsion Laboratory |
| LANL | Los Alamos National Laboratory |
| LETG | Low Energy Transmission Grating |
| LMC | Large Magellanic Cloud |
| LMXB | Low Mass X-ray Binary |
| LTI | Learning Technologies, Inc. |
| LTSA | Long Term Support in Astrophysics |
| MAST | Multimission Archive at Space Telescope |
| MESA | Math, Engineering, Science, Achievement |
| MOO | Mission of Opportunity |
| MOS | MOS style EPIC CCD detector |
| MSSL | Mullard Space Science Laboratory |
| NAS | National Academy of Sciences |
| NASA | National Aeronautics and Space Administration |
| NLS1 | Narrow Line Seyfert 1 |
| NPS | North Polar Spur |
| NRC | National Research Council |
| NS | Neutron Star |
| NSF | National Science Foundation |
| NVO | National Virtual Observatory |
| OM | Optical Monitor |
| OSS | Office of Space Science |
| PDS | Power Density Spectrum |
| PGP | Pretty Good Privacy |
| PI | Principal Investigator |
| PIMMS | Portable, Interactive Multi-Mission Simulator |
| PN | PN style EPIC CCD detector |
| PNe | Planetary Nebulae |
| PSD | Power Spectral Density |
| PSF | Point Spread Function |
| PV | Pointing Verification |
| PWN | Pulsar Wind Nebula |
| QPO | Quasi-Periodic Oscillation |
| QSO | Quasi-Stellar Object |
| RASS | ROSAT All-Sky Survey |
| RGS | Reflection Grating Spectrometer |
| RMS | Root Mean Square |
| ROSAT | Röntgen Satellite |
| RPS | Remote Proposal System |
| RRC | Radiative Recombination Complexes |
| RTRD | Real Time Raw Data |
| RUP | Roseland University Prep |
| RXTE | Rossi X-ray Time Explorer |
| SAS | Science Analysis System |
| SDSS | Sloan Digital Sky Survey |
| SEU | Structure and Evolution of the Universe |
| SGR | Soft Gamma-ray Repeater |
| SMD | Science Mission Directorate |
| SMEX | Small Explorer |
| SN | Supernova |
| S/N | Signal to Noise |
| SNR | Supernova Remnant |
| SOC | Science Operations Center |
| SRON | Netherlands Institute for Space Research |
| SSB | Space Studies Board (of the NRC) |
| SSC | Survey Science Centre |
| SSU | Sonoma State University |
| STEM | Science, Technology, Engineering and Math |
| STScI | Space Telescope Science Institute |
| SWCX | Solar Wind Charge Exchange |
| SWIRE | Spitzer Wide-area Infrared Extragalactic Survey |
| TAX | Two-Absorber X-ray |
| TAXP | Transient Anomalous X-ray Pulsar |
| TOO | Target of Opportunity |
| UC | University of California |
| UCB | University of California, Berkeley |
| UCR | University of California, Riverside |
| UCSB | University of California, Santa Barbara |
| UK | United Kingdom |
| ULX | Ultra-Luminous X-ray source |
| US | United States |
| UV | Ultra Violet |
| VLT | Very Large Telescope |
| WR | Wolf-Rayet |
| XCS | X-ray Cluster Survey |
| XDINS | X-ray Dim Isolated Neutron Stars |
| XEST | XMM-Newton Extended Survey of Taurus |
| XID | X-ray source IDenfication program |
| XMM-Newton | Newton X-ray Multi-Mirror Observatory |
| XMM-ESAS | XMM-Newton Extended Source Analysis Software |
| XRB | X-ray Binary |
| XSA | XMM-Newton Science Archive |
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The command line arguments were:
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The translation was initiated by Michael Arida on 2008-03-14
counts,
emphasizing the need for high-quality data (Guainazzi et al. 2006).
as the selection criteria in the redshift range
to 0.183. This sample made optimal use of the
large XMM-Newton FOV, and provides nearly homogeneous X-ray
luminosity coverage for the full range from poor
clusters to the most massive objects in the Universe
keV, 
keV, and 
keV respectively.
The green outline shows the limits of the survey area.
The white ellipse represents the 
contour. All
sources have X-ray spectra and light curves.