J/MNRAS/472/308 Supernova remnants in M33: X-ray properties (Garofali+, 2017)
Supernova remnants in M33: X-ray properties as observed by XMM-Newton.
Garofali K., Williams B.F., Plucinsky P.P., Gaetz T.J., Wold B., Haberl F.,
Long K.S., Blair W.P., Pannuti T.G., Winkler P.F., Gross J.
<Mon. Not. R. Astron. Soc., 472, 308-333 (2017)>
=2017MNRAS.472..308G 2017MNRAS.472..308G (SIMBAD/NED BibCode)
ADC_Keywords: Supernova remnants; X-ray sources; Cross identifications; Optical
Keywords: catalogues - ISM: supernova remnants, Local Group
Abstract:
We have carried out a study of the X-ray properties of the supernova
remnant (SNR) population in M33 with XMM-Newton, comprising deep
observations of eight fields in M33 covering all of the area within
the D25 contours, and with a typical luminosity of 7.1x1034erg/s
(0.2-2.0keV). Here, we report our work to characterize the X-ray
properties of the previously identified SNRs in M33, as well as our
search for new X-ray detected SNRs. With our deep observations and
large field of view we have detected 105 SNRs at the 3σ level,
of which 54 SNRs are newly detected in X-rays, and three are newly
discovered SNRs. Combining XMM-Newton data with deep Chandra survey
data allows detailed spectral fitting of 15 SNRs, for which we have
measured temperatures, ionization time-scales and individual
abundances. This large sample of SNRs allows us to construct an X-ray
luminosity function, and compare its shape to luminosity functions
from host galaxies of differing metallicities and star formation rates
to look for environmental effects on SNR properties. We conclude that
while metallicity may play a role in SNR population characteristics,
differing star formation histories on short time-scales, and
small-scale environmental effects appear to cause more significant
differences between X-ray luminosity distributions. In addition, we
analyse the X-ray detectability of SNRs, and find that in M33 SNRs
with higher [SII]/Hα ratios, as well as those with smaller
galactocentric distances, are more detectable in X-rays.
Description:
Herein we utilize data from a deep survey of M33 using an 8 field
XMM-Newton mosaic that extends out to the D25 isophote. The point
source catalogue from this survey was published by W15
(Williams+, 2015, J/ApJS/218/9).
In addition to the catalogue of W15, we utilize high-resolution
observations from the Chandra ACIS Survey of M33 (ChASeM33, Tullmann+
2011, J/ApJS/193/31).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 125 218 All 218 SNR and SNR candidates in our sample
table3.dat 133 105 All 105 3σ SNRs detected in our sample
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See also:
B/chandra : The Chandra Archive Log (CXC, 1999-2014)
B/xmm : XMM-Newton Obs. Log (XMM-Newton Science Operation Center, 2012)
VII/272 : A catalogue of Galactic supernova remnants (Green, 2014)
J/ApJ/855/140 : MMT spectra of SNRs and SNR candidates in M33 (Long+, 2018)
J/A+A/585/A162 : X-ray supernova remnants in LMC (Maggi+, 2016)
J/ApJS/218/9 : Deep XMM-Newton survey of M33 (Williams+, 2015)
J/ApJ/795/170 : Sample SNRs for M31 and M33 (Jennings+, 2014)
J/ApJ/793/134 : M33 SNR candidates properties (Lee+, 2014)
J/ApJ/789/10 : M33 WR and Of-type Stars (Neugent+, 2014)
J/ApJS/212/21 : A deep Chandra ACIS survey of M83 (Long+, 2014)
J/ApJ/786/130 : Catalog of M31 SNR candidates (Lee+, 2014)
J/MNRAS/429/189 : SNRs in six nearby galaxies (Leonidaki+, 2013)
J/ApJS/203/8 : Optical SNR candidates in M83 (Blair+, 2012)
J/ApJS/193/31 : M33 Chandra ACIS survey: final catalog (Tullmann+, 2011)
J/ApJ/725/842 : New X-ray-selected SNRs with Chandra (Leonidaki+, 2010)
J/ApJS/187/495 : SNRs in M33 from optical and X-ray (Long+, 2010)
J/AJ/138/1243 : The star formation history of the LMC (Harris+, 2009)
J/ApJS/174/366 : Chandra ACIS survey of M33 (ChaSeM33) (Plucinsky+, 2008)
J/AJ/131/2478 : M31 and M33 UBVRI photometry (Massey+, 2006)
J/A+A/426/11 : XMM-Newton survey of M33 (Pietsch+, 2004)
J/ApJS/120/247 : Supernova remnants in M33 (Gordon+, 1999)
J/A+AS/114/215 : New SNR candidates in M31 (Magnier+, 1995)
J/ApJS/79/77 : Bell Lab. H I Survey - High Velocity Clouds (Stark+ 1992)
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- [GWP2017] ID number from this catalogue
9 A1 --- n_[GWP2017] Note on [GWP2017] (G1)
11- 13 I03 --- [LBW2010] [1/137]? ID number in L10
(Long+ 2010, J/ApJS/187/495)
15- 17 I3 --- [LL2014b] [1/199]? ID number in LL14
(Lee & Lee 2014, J/ApJ/793/134)
19 I1 h RAh Hour of right ascension (J2000)
21- 22 I2 min RAm Minute of right ascension (J2000)
24- 28 F5.2 s RAs Second of right ascension (J2000)
30 A1 --- DE- Sign of declination (J2000)
31- 32 I2 deg DEd Degree of declination (J2000)
34- 35 I2 arcmin DEm Arcminute of declination (J2000)
37- 41 F5.2 arcsec DEs Arcsecond of declination (J2000)
43- 47 I5 ct C0.2-2keV [1/59600] Source counts in
the 0.2-2.0keV band (G2)
49- 51 I3 ct e_C0.2-2keV [7/814] C0.2-2keV uncertainty
53- 60 E8.3 ct/s CR0.2-2keV [2.3e-05/0.6] Source count rates in
the 0.2-2.0keV band (G2)
62- 69 E8.3 ct/s e_CR0.2-2keV [8.6e-05/0.008] CR0.2-2keV uncertainty
71 A1 --- l_F0.2-2keV Upper limit flag on F0.2-2
73- 80 E8.3 mW/m2 F0.2-2keV [1e-17/5e-13] Fluxes in the 0.2-2.0keV band
in erg/s/cm2 (G2)
82 A1 --- l_F0.35-2keV Upper limit flag on F0.35-2
84- 91 E8.3 mW/m2 F0.35-2keV [5.8e-17/5e-13] Fluxes in the 0.35-2.0keV
band in erg/s/cm2 (G3)
93- 97 F5.1 pc DL10 [8/179]? Optical SNR sizes from L10
99-103 F5.1 pc DLL14 [10/100]? Optical SNR sizes from LL14
105-108 F4.2 [-] SII/HaL10 [0.2/1.7]? [SII]/Hα ratio from L10 (1)
110-113 F4.2 [-] SII/HaLL14 [0.3/1.6]? [SII]/Hα ratio from LL14 (1)
115-119 F5.2 [10-7W] logLHaL10 [34.9/37.5]? log of the Hα luminosity
from L10
121-125 F5.2 [10-7W] logLHaLL14 [34.7/37.3]? log of the Hα luminosity
from LL14 in erg/s
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Note (1): Used for optical selection of candidates.
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Byte-by-byte Description of file: table3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 A7 --- [GWP2017] ID number from this catalogue
9 A1 --- n_[GWP2017] Note on [GWP2017] (G1)
11 I1 h RAh Hour of right ascension (J2000)
13- 14 I2 min RAm Minute of right ascension (J2000)
16- 20 F5.2 s RAs Second of right ascension (J2000)
22 A1 --- DE- Sign of declination (J2000)
23- 24 I2 deg DEd Degree of declination (J2000)
26- 27 I2 arcmin DEm Arcminute of declination (J2000)
29- 33 F5.2 arcsec DEs Arcsecond of declination (J2000)
35- 39 I5 ct C0.2-2keV [52/21032] Source counts in
the 0.2-2.0keV band (G2)
41- 43 I3 ct e_C0.2-2keV [13/531] C0.2-2keV uncertainty
45- 49 I5 ct C0.35-2keV [19/20152] Source counts in
the 0.35-2keV band (G3)
51- 53 I3 ct e_C0.35-2keV [13/512] C0.35-2keV uncertainty
55- 58 I4 ct C0.3-0.7keV [1/8698] Source counts in
the 0.3-0.7keV (soft) band (1)
60- 62 I3 ct e_C0.3-0.7keV [6/351] C0.3-0.7keV uncertainty
64- 67 I4 ct C0.7-1.1keV [7/9787] Source counts in
the 0.7-1.1keV (medium) band (1)
69- 71 I3 ct e_C0.7-1.1keV [6/303] C0.7-1.1keV uncertainty
73- 76 I4 ct C1.1-4.2keV [8/2592] Source counts in
the 1.1-4.2keV (hard) band (1)
78- 80 I3 ct e_C1.1-4.2keV [6/475] C1.1-4.2keV uncertainty
82- 86 F5.2 --- HR1 [-0.8/0.9] Hardness ratio in the 0.3-0.7,
0.7-1.1 and 1.1-4.2 keV bands
(HR1=(M-S)/(H+M+S))
88- 91 F4.2 --- e_HR1 [0/0.5] HR1 uncertainty
93- 97 F5.2 --- HR2 [-0.9/0.8] Hardness ratio in the 0.3-0.7,
0.7-1.1 and 1.1-4.2keV bands
(HR2=(H-M)/(H+M+S))
99-102 F4.2 --- e_HR2 [0/0.6] HR2 uncertainty
104-108 F5.2 --- HR1XMM [-1/1]? Hardness ratio from the 0.2-0.5,
0.5-1.0 and 1.0-2.0keV bands
(HR1XMM=(M-S)/(S+M))
110-113 F4.2 --- e_HR1XMM [0/0.6]? HR1XMM uncertainty
115-119 F5.2 --- HR2XMM [-0.9/1]? Hardness ratio from the 0.2-0.5,
0.5-1.0 and 1.0-2.0keV bands
(HR2XMM=(H-M)/(H+M))
121-124 F4.2 --- e_HR2XMM [0/0.8]? HR2XMM uncertainty
126-133 A8 --- DetL10 Measurement level in L10: 3σ, 2σ
or upper limit (<)
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Note (1): Source counts and errors in the 0.3-0.7 (soft), 0.7-1.1 (medium) and
1.1-4.2 (hard) keV bands, which are used for computing the HRs shown
in Fig. 7.
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Global notes:
Note (G1): Note as follows:
c = Flux is contaminated by nearby bright X-ray source, but source has a
previous X-ray detection. Flux is an upper limit.
e = Unrealistic source count errors from emldetect in at least one individual
band. Source count errors pegged to total count values.
n = Determined to be a non-detection via by-eye catalogue checking.
Flux is an upper limit.
t = Total counts in the full band are discrepant by a factor of two from the
summation of counts in each individual band due an emldetect merging
issue. Total counts in the 0.2-2.0keV band are reported as the sum of
counts in the 0.2-0.5, 0.5-1.0 and 1.0-2.0keV band.
x = Flux is contaminated by nearby bright X-ray source, but source does not
have a previous X-ray detection. Flux is an upper limit.
Note (G2): Used for detection.
Note (G3): Used for comparison to L10 (Long+ 2010, J/ApJS/187/495).
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History:
From electronic version of the journal
(End) Emmanuelle Perret [CDS] 21-Feb-2019