J/A+A/633/A42 Calibration list (Sanders+, 2020)
Measuring bulk flows of the intracluster medium in the Perseus and Coma galaxy
clusters using XMM-Newton.
Sanders J.S., Dennerl K., Russell H.R., Eckert D., Pinto C., Fabian A.C.,
Walker S.A., Tamura T., ZuHone J., Hofmann F.
<Astron. Astrophys. 633, A42 (2020)>
=2020A&A...633A..42S 2020A&A...633A..42S (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, galaxy ; X-ray sources
Keywords: galaxies: clusters: intracluster medium -
X-rays: galaxies: clusters -
galaxies: clusters: individual: Coma cluster -
galaxies: clusters: individual: Perseus cluster -
techniques: imaging spectroscopy
Abstract:
We demonstrate a novel technique for calibrating the energy scale of
the EPIC-pn detector on XMM-Newton, which allows us to measure bulk
flows in the intracluster medium (ICM) of the Perseus and Coma galaxy
clusters. The procedure uses the fluorescent instrumental background
lines present in all observations, in particular, Cu-Kalpha. By
studying their spatial and temporal variations, in addition to
incorporating calibration observations, we refined the absolute energy
scale of the detector to better than 150km/s at the Fe-K line, a
large improvement over the nominal calibration accuracy of 550km/s.
With our calibration, we mapped the bulk motions over much of the
central 1200 and 800kpc of Perseus and Coma, respectively, in spatial
regions down to 65 and 140kpc size. We cross-checked our procedure by
comparing our measurements with those found in Perseus by Hitomi for
an overlapping 65 kpc square region, finding consistent results. For
Perseus, there is a relative line-of-sight velocity increase of
480±210km/s (1sigma) at a radius of 250kpc east of the nucleus.
This region is associated with a cold front, providing direct evidence
of the ICM sloshing in the cluster potential well. Assuming the
intrinsic distribution of bulk motions is Gaussian, its width is
214±85km/s, excluding systematic uncertainties. Removing the
sloshing region, this is reduced to 20-150km/s, which is similar in
magnitude to the Hitomi line width measurements in undisturbed
regions. In Coma, the line-of-sight velocity of the ICM varies between
the velocities of the two central galaxies. Maps of the gas velocity
and metallicity provide clues about the merger history of the Coma,
with material to the north and east of the cluster core having a
velocity similar to NGC 4874, while that to the south and west has
velocities close to NGC 4889. Our results highlight the difference
between a merging system, such as Coma, where we observe a ∼1000 km/s
range in velocity, and a relatively relaxed system, such as Perseus,
with much weaker bulk motions.
Description:
List of XMM-Newton EPIC-pn input datasets which went into the
characterisation of the detector energy calibration. Provided are a
list of normal astronomical observations, and a list of calibration
observations. Included in the tables are the XMM revolution for an
observation, its identifier (OBSID), detector mode and cleaned
exposure time. For the calibration observations we also include the
exposure identifier. Detector modes are either FF or F, for full-frame
mode, or EFF or E for extended-full-frame mode.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
cal.dat 29 108 Calibration observation list (table A1)
data.dat 23 1677 Astronomical observation list (table A2)
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Byte-by-byte Description of file: cal.dat
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Bytes Format Units Label Explanations
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1- 4 I4 --- Revolut Observation revolution
6- 15 A10 --- OBSID Observation identifier
17- 19 A3 --- ExposID Exposure identifier
21- 23 A3 --- Mode Detector mode (FF/EFF)
25- 29 F5.1 ks Exposure Exposure time after cleaning
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Byte-by-byte Description of file: data.dat
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Bytes Format Units Label Explanations
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1- 4 I4 --- Revolut Observation revolution
6- 15 A10 --- OBSID Observation identifier
17 A1 --- Mode Detector mode (F/E)
19- 23 F5.1 ks Exposure Exposure time after cleaning
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Acknowledgements:
Jeremy Sanders, jsanders(at)mpe.mpg.de
(End) Jeremy Sanders [MPE, Germany], Patricia Vannier [CDS] 04-Dec-2019