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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
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:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 94 19 Galaxy parameters tables.dat 79 356 SNRs in the 19 nearby galaxies sample
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
Bytes Format Units Label Explanations
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) 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)
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) and the inclination for NGC 2366 from Hunter et al. (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) and Schlegel et al. (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), 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). Note (4): As determined by Anantharamaiah et al. (2000ApJ...537..613A), but converted to the IMF used in the Calzetti et al. (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%.
Byte-by-byte Description of file: tables.dat
Bytes Format Units Label Explanations
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
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 ; <[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; <[CW2009] NNNNN-NN> in Simbad; tables 7, 9, 10, and 15, respectively). * N300 (table 8 of the paper): Pannuti et al. (2000ApJ...544..780P; <[PDL2000] RNN> in Simbad and <[BL97] N300-ANN>). * M82 (table 11 of the paper): Allen & Kronberg (1998ApJ...502..218A) and McDonald et al. (2002MNRAS.334..912M; <[MMW2002] SS.ss+SS.s> in Simbad). * M81 (table 12 of the paper): Kaufman et al. (1987ApJ...319...61K; <[KBK87] NNN> in Simbad). * N7793 (table 13 of the paper): Pannuti et al. (2002ApJ...565..966P; <[PDL2002] NGC 7793 RN> and <[BL97] N7793-SNN> in Simbad). * N253 (table 14 of the paper): Ulvestad & Antonucci (1997ApJ...488..621U; <[AU88] S.ss-SS.s> in Simbad) and Ulvestad (2000AJ....120..278U; <[U2000] NN> in Simbad). * M83 (table 16): Maddox et al. (2006AJ....132..310M; <[MCK2006] NN> in Simbad) * N4736 (table 17 of the paper): Duric & Dittmar (1988ApJ...332L..67D; <[DD88] NN> for Simbad). * N6946 (table 18): Lacey et al. (1997ApJS..109..417L; <[LDG97] NNN> in Simbad) * N4258 (table 19 of the paper): Hyman et al. (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; <[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.
History: From electronic version of the journal
(End) Emmanuelle Perret [CDS] 13-Oct-2011
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