J/ApJS/233/20 CGM-MASS. II. New XMM data for 6 spirals (Li+, 2017)
The Circum-Galactic Medium of MASsive Spirals.
II. Probing the nature of hot gaseous halo around the most massive isolated
spiral galaxies.
Li J.-T., Bregman J.N., Wang Q.D., Crain R.A., Anderson M.E., Zhang S.
<Astrophys. J. Suppl. Ser., 233, 20 (2017)>
=2017ApJS..233...20L 2017ApJS..233...20L
ADC_Keywords: Galaxies, nearby; X-ray sources; Redshifts; Intergalactic medium
Keywords: galaxies: formation ; galaxies: halos ; galaxies: spiral ;
intergalactic medium ; X-rays: galaxies
Abstract:
We present the analysis of the XMM-Newton data of the Circum-Galactic
Medium of MASsive Spirals (CGM-MASS) sample of six extremely massive
spiral galaxies in the local universe. All the CGM-MASS galaxies have
diffuse X-ray emission from hot gas detected above the background
extending ~(30-100)kpc from the galactic center. This doubles the
existing detection of such extended hot CGM around massive spiral
galaxies. The radial soft X-ray intensity profile of hot gas can be
fitted with a β-function, with the slope typically in the range
of β=0.35-0.55. This range, as well as those β values
measured for other massive spiral galaxies, including the Milky Way
(MW), are in general consistent with X-ray luminous elliptical
galaxies of similar hot gas luminosity and temperature, and with those
predicted from a hydrostatic- isothermal gaseous halo. Hot gas in such
a massive spiral galaxy tends to have temperature comparable to its
virial value, indicating the importance of gravitational heating. This
is in contrast to lower mass galaxies, where hot gas temperature tends
to be systematically higher than the virial one. The ratio of the
radiative cooling to free fall timescales of hot gas is much larger
than the critical value of ∼10 throughout the entire halos of all the
CGM-MASS galaxies, indicating the inefficiency of gas cooling and
precipitation in the CGM. The hot CGM in these massive spiral galaxies
is thus most likely in a hydrostatic state, with the feedback material
mixed with the CGM, instead of escaping out of the halo or falling
back to the disk. We also homogenize and compare the halo X-ray
luminosity measured for the CGM-MASS galaxies and other galaxy samples
and discuss the "missing" galactic feedback detected in these massive
spiral galaxies.
Description:
We have analyzed the XMM-Newton observations of the Circum-Galactic
Medium of MASsive Spirals (CGM-MASS) galaxies, following the same
procedure as presented in Paper I (Li+ 2016ApJ...830..134L 2016ApJ...830..134L).
The five galaxies selected in Paper I have been observed by XMM-Newton
in AO-13 and AO-14, with a total exposure time of ∼0.5Ms (the program
has been approved in AO-13; PI: Jiang-Tao Li).
Information on the XMM-Newton data used in this paper is summarized in
Table 5 (observations span 2008 Dec to 2015 Jun).
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . this file
table1.dat 59 6 Properties of the Circum-Galactic Medium of MASsive
Spirals (CGM-MASS) galaxies
table5.dat 56 7 XMM-Newton data of the CGM-MASS galaxies
table6.dat 119 73 Cross-identified sources around the CGM-MASS galaxies
table7.dat 422 11550 The full source catalog
table8.dat 73 5 X-ray properties of the nuclear regions of
the CGM-MASS galaxies
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See also:
B/xmm : XMM-Newton Observation Log (XMM-Newton Science Operation Center, 2012)
VII/233 : The 2MASS Extended sources (IPAC/UMass, 2003-2006)
J/MNRAS/371/147 : XMM-Newton observation of NGC 2613 (Li+, 2006)
J/MNRAS/376/960 : X-ray emission from the Sombrero galaxy (NGC4594) (Li+, 2007)
J/MNRAS/390/59 : X-ray sources in NGC 5775 (Li+, 2008)
J/ApJ/706/693 : X-ray sources in NGC 5866 (Li+, 2009)
J/ApJ/795/158 : The MASSIVE survey : 116 candidate galaxies (Ma+, 2014)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 A11 --- Gal Galaxy name
13- 17 F5.2 kpc/arcmin Scale [15.1/27.45] Scale
19- 22 F4.2 10+11Msun M* [1.4/6] Stellar mass (1)
24- 27 F4.2 10+11Msun e_M* [0.08/0.8] Negative uncertainty on M*
29- 32 F4.2 10+11Msun E_M* [0.01/0.2] Positive uncertainty on M*
34- 38 F5.3 Msun/Lsun M*/LK [0.5/1.2] K-band mass-to-light ratio (2)
40- 43 F4.2 Msun/yr SFR [0.3/4] Star Formation Rate (3)
45- 48 F4.2 Msun/yr e_SFR [0.06/0.2] SFR uncertainty
50- 54 F5.2 10+11Msun MTF [4/16.1] Total baryon mass MTF (4)
56- 59 F4.2 10+11Msun e_MTF [0.6/2]? MTF uncertainty
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Note (1): The stellar mass, M*, is measured from the 2MASS K-band luminosity;
updated from Paper I (Li+ 2016ApJ...830..134L 2016ApJ...830..134L).
Note (2): The K-band mass-to-light ratio (M*/LK) of the galaxies is estimated
from the inclination, redshift, and Galactic extinction corrected
B-V color, except for UGCA 145, for which the corrected B-R color is
used (Section 2.1); updated from Paper I (Li+ 2016ApJ...830..134L 2016ApJ...830..134L).
Note (3): SFR is estimated from the WISE 22um luminosity (Section 2.1); updated
from Paper I (Li+ 2016ApJ...830..134L 2016ApJ...830..134L).
Note (4): The total baryon mass, MTF, is estimated from the inclination
corrected rotation velocity Vrot and the baryonic Tully-Fisher
relation (Bell & de Jong 2001ApJ...550..212B 2001ApJ...550..212B), and is used to produce
Figure 9(b); updated from Paper I (Li+ 2016ApJ...830..134L 2016ApJ...830..134L).
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 A11 --- Gal Galaxy name
13 I1 --- m_Gal ? Indicate a second observation for NGC 550
15- 23 I9 --- ObsID XMM-Newton observation ID
25- 35 A11 "Y/M/D" Date Start date of observation
37- 41 F5.1 ks tXMM [45.5/124] Total exposures of the XMM-Newton
observations
43- 46 F4.1 ks teffM1 [41.3/85] Cleaned effective exposure times
of MOS-1
48- 51 F4.1 ks teffM2 [42/93] Cleaned effective exposure times of MOS-2
53- 56 F4.1 ks teffPN [15.3/56] Cleaned effective exposure times of PN
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Byte-by-byte Description of file: table6.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 A11 --- Gal Galaxy name
13- 16 F4.2 10+31W L0.3-7.2 [1.8/6] 0.3-7.2keV limit in 1038erg/s
18- 20 A3 --- ID Source ID
22- 51 A30 --- Name Identified source name
53- 54 I2 h RAh Hour of right ascension (J2000)
56- 57 I2 min RAm Minute of right ascension (J2000)
59- 62 F4.1 s RAs Second of right ascension (J2000)
64 A1 --- DE- Sign of declination (J2000)
65- 66 I2 deg DEd Degree of declination (J2000)
68- 69 I2 arcmin DEm Arcminute of declination (J2000)
71- 72 I2 arcsec DEs Arcsecond of declination (J2000)
74- 86 A13 --- Type Type of the source
88- 95 F8.6 --- z [0.006/2.8]? Redshift
97-119 A23 --- Shape X-ray shape
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Byte-by-byte Description of file: table7.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 A11 --- Gal Galaxy identifier (1)
13 I1 --- m_Gal ? Indicate first or second observation
for NGC 550
15- 17 I3 --- ML-ID [1/203] EMLDETECT source number
19- 21 I3 --- Box-ID [1/320] Corresponding EBOXDETECT input source
number
23- 23 I1 --- Inst [0/3]? XMM instrument (2)
25- 25 I1 --- Band [0/2] Energy band number (3)
27- 29 I3 --- Clust [1/307] Cluster identifier (4)
31- 42 E12.6 ct Cts [0/20931]? Source counts
44- 55 E12.6 ct e_Cts [0/168]? Uncertainty in Cts
57- 68 E12.6 pix Xpix Source X pixel coordinate
70- 81 E12.6 pix e_Xpix Uncertainty in Xpix
83- 94 E12.6 pix Ypix Source Y pixel coordinate
96-107 E12.6 pix e_Ypix Uncertainty in Ypix
109-120 E12.6 --- Det [0/64071]? Likelihood of detection
122-133 E12.6 ct/pix Bkgrd [1e-05/2.2]? Background at source
135-146 E12.6 s Exp [0.006/93203]? Vignetting corrected exposure
at source
148-159 E12.6 mW/m2 Flux [0/1.5e-12]? Source flux; erg/s/cm2
161-172 E12.6 mW/m2 e_Flux ? Uncertainty in Flux
174-185 E12.6 ct/s Rate [0/0.7]? Source count rate
187-198 E12.6 ct/s e_Rate [0/0.02]? Uncertainty in Rate
200-217 E18.12 deg RAdeg Source Right Ascension in
decimal degrees (J2000)
219-237 E19.12 deg DEdeg Declination in decimal degrees (J2000)
239-250 E12.6 deg PosErr [0.06/4.1] Uncertainty in source position
252-269 E18.12 deg GLON Source galactic longitude
271-289 E19.12 deg GLAT Source galactic latitude
291-294 I4 pix RAWX ? Raw source X pixel coordinate
296-299 I4 pix RAWY ? Raw source Y pixel coordinate
301-312 E12.6 deg OAngle [0.1/18]? Off axis angle
314-317 I4 --- CCD [1/12]? Chip number
319-331 E13.6 --- HR ? Hardness ratio (5)
333-344 E12.6 --- e_HR [0.008/15160]? Uncertainty in HR
346-357 E12.6 pix CutRad [5.5/17.1] Source cut out radius
359-370 E12.6 pix Mask ? PSF weighted on-chip fraction
372-383 E12.6 --- EEF [0.6/0.9]? Encircled energy fraction
385-396 E12.6 --- Vig [0/1.1]? Vignetting
398-409 E12.6 s OnTime [18239/93882]? Integration time, not
vignetting corrected
411-422 E12.6 arcsec Sep [11.8/228.1] Distance to nearest neighbor
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Note (1): There are two observations of NGC550 with comparable exposure time,
so the source detection is conducted separately for them, and users
may examine the variations of the sources.
Note (2): Instrument as follows:
1 = PN;
2 = MOS1;
3 = MOS2.
Note (3): Either the band number or 0 for the summary band.
Note (4): Sources fit simultaneously have same number.
Note (5): Where HR=(H-S)/(H+S) and H is the hard (2-7.2keV) band and
S is the soft (0.3-2keV) band.
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Byte-by-byte Description of file: table8.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- Gal Galaxy name
13- 17 F5.2 10+32W Lx [8.1/27.7]? X-ray luminosity LX,power (1)
19- 22 F4.2 10+32W e_Lx [0.7/3]? Lx negative uncertainty
24- 27 F4.2 10+32W E_Lx [0.7/3.3]? Lx positive uncertainty
29- 33 F5.2 10+32W LxAPEC [0.5/14] X-ray luminosity LX,APEC (1)
35- 38 F4.2 10+32W e_LxAPEC [0.1/1.2] LxAPEC negative uncertainty
40- 43 F4.2 10+32W E_LxAPEC [0.1/1.1] LxAPEC positive uncertainty
45- 48 F4.2 --- Gamma [1.2/1.5]? Photon index
50- 53 F4.2 --- e_Gamma [0.1/0.2]? Negative uncertainty in Gamma
55- 58 F4.2 --- E_Gamma [0.1/0.3]? Positive uncertainty in Gamma
60- 63 F4.2 keV kT [0.3/0.9] Hot gas temperature
65- 68 F4.2 keV e_kT [0.03/0.3] Negative uncertainty in kT
70- 73 F4.2 keV E_kT [0.04/0.2] Positive uncertainty in kT
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Note (1): The net (background and stellar components subtracted) spectra of the
regions are modeled with a power law plus a thermal plasma (APEC), if
needed. The key parameters of these two components are represented by
Γ (photon index) and kT (hot gas temperature), while their
corresponding absorption-corrected luminosities are given in the
0.3-8keV and 0.5-2keV bands, respectively.
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History:
From electronic version of the journal
References:
Li et al. Paper I. 2016ApJ...830..134L 2016ApJ...830..134L
Li et al. Paper II. 2017ApJS..233...20L 2017ApJS..233...20L This catalog
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 19-Feb-2018