J/ApJ/703/370 Radio SNRs in nearby galaxies (Chomiuk+, 2009)
A universal luminosity function for radio supernova remnants.
Chomiuk L., Wilcots E.M.
<Astrophys. J., 703, 370-389 (2009)>
=2009ApJ...703..370C 2009ApJ...703..370C
ADC_Keywords: Supernova remnants ; Radio continuum ; Galaxies, nearby
Keywords: acceleration of particles - magnetic fields -
radio continuum: galaxies - supernova remnants
Abstract:
We compile radio supernova remnant (SNR) samples from the literature
for 19 nearby galaxies ranging from the SMC to Arp 220, and use this
data to constrain the SNR luminosity function (LF) at 20cm. We find
that radio SNR populations are strikingly similar across galaxies. The
LF can be described as a power law with constant index and scaling
proportional to a galaxy's star formation rate (SFR). Unlike previous
authors, we do not find any dependence of SNR luminosity on a galaxy's
global interstellar medium density. The observed correlation between
the luminosity of a galaxy's brightest SNR and a galaxy's SFR can be
completely explained by statistical effects, wherein galaxies with
higher SFR more thoroughly sample the high-luminosity end of the SNR
LF. The LF is well fitted by a model of SNR synchrotron emission which
includes diffusive shock acceleration and magnetic field
amplification, if we assume that all remnants are undergoing adiabatic
expansion, the densities of star-forming regions are similar across
galaxies, and the efficiency of cosmic ray production is constant.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 94 19 Galaxy parameters
tables.dat 79 356 SNRs in the 19 nearby galaxies sample
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See also:
VII/237 : HYPERLEDA. I. Catalog of galaxies (Paturel+, 2003)
VII/109 : IRAS Observations of Large Optical Galaxies (Rice+, 1988)
VII/155 : Third Reference Cat. of Bright Galaxies (RC3) (de Vaucouleurs+ 1991)
J/ApJS/187/495 : SNRs in M33 from optical and X-ray (Long+, 2010)
J/ApJS/178/247 : Hα and [NII] survey in local 11 Mpc (Kennicutt+, 2008)
J/AJ/133/2559 : Compact radio sources in spiral galaxies. II. (Maddox+, 2007)
J/A+A/462/507 : AMIGA III. IRAS data (Lisenfeld+, 2007)
J/MNRAS/355/44 : ATCA SMC Radio Continuum Source. II. (Payne+, 2004)
J/AJ/126/1607 : IRAS Revised Bright Galaxy Sample (Sanders+, 2003)
J/ApJS/120/247 : Supernova remnants in M33 (Gordon+, 1999)
J/A+AS/130/421 : Radio continuum study of the MC (Filipovic+ 1998)
J/A+AS/111/311 : Radio continuum study of the MC (Filipovic+, 1995)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 8 A8 --- Gal Galaxy name
10- 11 I2 h RAh NED Hour of right ascension (J2000)
13- 14 I2 min RAm NED Minute of right ascension (J2000)
16- 19 F4.1 s RAs NED Second of right ascension (J2000)
21 A1 --- DE- NED Sign of declination (J2000)
22- 23 I2 deg DEd NED Degree of declination (J2000)
25- 26 I2 arcmin DEm NED Arcminute of declination (J2000)
28- 29 I2 arcsec DEs NED Arcsecond of declination (J2000)
31- 35 F5.1 arcmin aMaj Major axis
37- 41 F5.1 arcmin bMin Minor axis
43- 44 I2 deg i Inclination (1)
46- 55 A10 --- TType Morphological type
57 A1 --- r_TType [f] f: From de Vaucouleurs & Freeman
(1972VA.....14..163D 1972VA.....14..163D)
59- 63 F5.2 Mpc Dist Distance from Kennicutt et al. (2008,
Cat. J/ApJS/178/247)
65- 69 F5.3 Mpc e_Dist ? Distance uncertainty
70 A1 --- n_Dist [g] g: Calculated assuming H0=75km/s/Mpc
72- 76 F5.1 mag BMAG Absolute B-band magnitude from Kennicutt et
al. (2008, Cat. J/ApJS/178/247)
78 A1 --- n_BMAG [h] BMAG derived from RC3 (2)
80- 85 F6.2 Msun/yr SFR Star formation rate (3)
86 A1 --- n_SFR [i] SFR converted to Calzetti et al. (4)
88- 94 F7.3 Msun/pc3 rau Average ISM densities in SNR survey areas (5)
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Note (1): From HyperLeda (Paturel et al. 2003, Cat. VII/237), except the values
for the Magellanic Clouds which come from Groenewegen
(2000A&A...363..901G 2000A&A...363..901G) and the inclination for NGC 2366 from Hunter et
al. (2001ApJ...559..225H 2001ApJ...559..225H).
Note (2): Calculated using the RC3 B mag as provided by NED, the average of the
foreground extinctions in Burstein & Heiles (1978ApJ...225...40B 1978ApJ...225...40B)
and Schlegel et al. (1998ApJ...500..525S 1998ApJ...500..525S), and a distance of 77Mpc.
Note (3): SFRs are calculated using a combination of Hα and 25um fluxes as
calibrated by Calzetti et al. (2007ApJ...666..870C 2007ApJ...666..870C), and using
Hα luminosities from Kennicutt et al. (2008,
Cat. J/ApJS/178/247), and 25um IRAS fluxes from the following
references in order of preference: Sanders et al. (2003,
Cat. J/AJ/126/1607), Rice et al. (1988, Cat. VII/109), Lisenfeld et
al. (2007, Cat. J/A+A/462/507), and Moshir et al.
(1992ifss.book.....M 1992ifss.book.....M).
Note (4): As determined by Anantharamaiah et al. (2000ApJ...537..613A 2000ApJ...537..613A),
but converted to the IMF used in the Calzetti et al.
(2007ApJ...666..870C 2007ApJ...666..870C) calibration.
Note (5): Rough estimate of the average ISM densities in SNR survey areas,
calculated as described in Section 3. A constant scale height is
assumed for all galaxies, and therefore the uncertainty on these
calculations is at least 50%.
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Byte-by-byte Description of file: tables.dat
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Bytes Format Units Label Explanations
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1- 8 A8 --- Gal Galaxy name
10- 23 A14 --- ID SNR identification (1)
24 A1 --- f_ID [*] *: SNR is in the complete sample for this
galaxy (2)
26- 27 I2 h RAh Hour of right ascension (J2000)
29- 30 I2 min RAm Minute of right ascension (J2000)
32- 38 F7.4 s RAs Second of right ascension (J2000)
40 A1 --- DE- Sign of declination (J2000)
41- 42 I2 deg DEd Degree of declination (J2000)
44- 45 I2 arcmin DEm Arcminute of declination (J2000)
47- 52 F6.3 arcsec DEs Arcsecond of declination (J2000)
54- 60 F7.2 mJy S1.4 Flux density at 1.45GHz
62- 67 F6.2 mJy e_S1.4 S1.4 uncertainty
69 A1 --- l_alpha Limit flag on alpha
70- 74 F5.2 --- alpha Spectral index α
76- 79 F4.2 --- e_alpha ? alpha uncertainty
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Note (1): The different identifications follow the references:
* LMC (table 3 of the paper): Filipovic et al., 1995, Cat. J/A+AS/111/311;
<[FHW95] LMC BHHMM-DDMM> in Simbad.
* SMC (table 4 of the paper): Payne et al. (2004, Cat. J/MNRAS/355/44);
<[FBR2002] JHHMMSS+DDMMSS> in Simbad).
* IC 10 (table 5 of the paper): Yang & Skillman (1993AJ....106.1448Y 1993AJ....106.1448Y ;
<[HL90] NNNa> in Simbad).
* M33 (table 6 of the paper): Gordon et al. (1999, Cat. J/ApJS/120/247;
<[GDK99] NNN> in Simbad).
* N1569, N4214, N2366, N4449: Chomiuk & Wilcots (2009AJ....137.3869C 2009AJ....137.3869C;
<[CW2009] NNNNN-NN> in Simbad; tables 7, 9, 10, and 15, respectively).
* N300 (table 8 of the paper): Pannuti et al. (2000ApJ...544..780P 2000ApJ...544..780P;
<[PDL2000] RNN> in Simbad and <[BL97] N300-ANN>).
* M82 (table 11 of the paper): Allen & Kronberg (1998ApJ...502..218A 1998ApJ...502..218A) and
McDonald et al. (2002MNRAS.334..912M 2002MNRAS.334..912M; <[MMW2002] SS.ss+SS.s> in Simbad).
* M81 (table 12 of the paper): Kaufman et al. (1987ApJ...319...61K 1987ApJ...319...61K;
<[KBK87] NNN> in Simbad).
* N7793 (table 13 of the paper): Pannuti et al. (2002ApJ...565..966P 2002ApJ...565..966P;
<[PDL2002] NGC 7793 RN> and <[BL97] N7793-SNN> in Simbad).
* N253 (table 14 of the paper): Ulvestad & Antonucci (1997ApJ...488..621U 1997ApJ...488..621U;
<[AU88] S.ss-SS.s> in Simbad) and Ulvestad (2000AJ....120..278U 2000AJ....120..278U;
<[U2000] NN> in Simbad).
* M83 (table 16): Maddox et al. (2006AJ....132..310M 2006AJ....132..310M; <[MCK2006] NN> in Simbad)
* N4736 (table 17 of the paper): Duric & Dittmar (1988ApJ...332L..67D 1988ApJ...332L..67D;
<[DD88] NN> for Simbad).
* N6946 (table 18): Lacey et al. (1997ApJS..109..417L 1997ApJS..109..417L; <[LDG97] NNN> in Simbad)
* N4258 (table 19 of the paper): Hyman et al. (2001ApJ...551..702H 2001ApJ...551..702H;
<[HCW2001] NNa> in Simbad).
* M51 (table 20 of the paper): Maddox et al. (2007, Cat. J/AJ/133/2559;
<[MCK2007] NNN> in Simbad).
* Arp220 (table 21 of the paper): Parra et al. (2007ApJ...659..314P 2007ApJ...659..314P;
<[LDT2006] WNN> in Simbad).
Note (2): The observations of each galaxy in our sample have distinct
limitations, and therefore only a subset of the SNRs described in
Section 2.2 can be considered to be in complete samples. We define
completeness in terms of SNR spectral luminosity using a method
developed by Gordon et al. (1999, Cat. J/ApJS/120/247) on the M33
SNR LF. Our definition of completeness appears to be conservative,
and unfortunately limits quite drastically the number of SNRs in our
sample for some galaxies. In total, we have 259 SNRs in complete
samples across the 18 sample galaxies, and four SNRs in the Arp 220
complete sample. See Section 2.4 for more explanation.
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History:
From electronic version of the journal
(End) Emmanuelle Perret [CDS] 13-Oct-2011