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J/ApJS/203/8            Optical SNR candidates in M83            (Blair+, 2012)

The Magellan/IMACS catalog of optical supernova remnant candidates in M83. Blair W.P., Winkler P.F., Long K.S. <Astrophys. J. Suppl. Ser., 203, 8 (2012)> =2012ApJS..203....8B
ADC_Keywords: Galaxies, optical ; Supernova remnants ; Cross identifications Keywords: galaxies: individual (M83) - galaxies: ISM - ISM: supernova remnants Abstract: We present a new optical imaging survey of supernova remnants (SNRs) in M83 (NGC 5236), using data obtained with the Magellan I 6.5m telescope and IMACS instrument under conditions of excellent seeing. Using the criterion of strong [SII] emission relative to Hα, we confirm all but three of the 71 SNR candidates listed in our previous survey, and expand the SNR candidate list to 225 objects, more than tripling the earlier sample. Comparing the optical survey with a new deep X-ray survey of M83 with Chandra, we find that 61 of these SNR candidates have X-ray counterparts. We also identify an additional list of 46 [OIII]-selected nebulae for follow-up as potential ejecta-dominated remnants, seven of which have associated X-ray emission that makes them strong candidates. Some of the other [OIII]-bright objects could also be normal interstellar medium (ISM) dominated SNRs with shocks fast enough to doubly ionize oxygen, but with Hα and [SII] emission faint enough to have been missed. A few of these objects may also be HII regions with abnormally high [OIII] emission compared with the majority of M83 HII regions, compact nebulae excited by young Wolf-Rayet stars, or even background active galactic nuclei. The SNR Hα luminosity function in M83 is shifted by a factor of ∼4.5 times higher than for M33 SNRs, indicative of a higher mean ISM density in M83. We describe the search technique used to identify the SNR candidates and provide basic information and finder charts for the objects. Description: We observed M83 from the 6.5m Magellan-I (Baade) telescope at the Las Campanas Observatory (LCO), using the IMACS instrument in its f/4.3 direct-imaging mode, on the nights of 2009 April 26 and 27 (UT). We carried out imaging in [OIII], Hα, and [SII] emission lines, plus green and red continuum bands for subtracting stars to better reveal the nebular emission. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table2.dat 90 225 ISM-dominated supernova remnants and candidates; updated version from the erratum published in 2017, ApJS, 229, 43 table3.dat 90 46 [OIII]-selected objects and supernova remnant candidates; updated version from the erratum (2017, ApJS, 229, 43)
See also: J/ApJS/212/21 : A deep Chandra ACIS survey of M83 (Long+, 2014) J/A+A/518/A29 : Distribution of WR stars in 2 nearby galaxies (Leloudas+, 2010) J/ApJ/706/553 : Fluxes in nearby star-forming galaxies (Boquien+, 2009) J/ApJ/700/654 : Keck spectroscopy of extragalactic HII regions (Esteban+ 2009) J/A+A/439/265 : Wolf-Rayet population in M83 (Hadfield+, 2005) J/A+A/410/53 : M83 X-ray sources (Soria+, 2003) Byte-by-byte Description of file: table[23].dat
Bytes Format Units Label Explanations
1- 3 I3 --- Seq [1/346] Object running sequence number (1) 5 A1 --- f_Seq Flag on Seq (2) 7- 8 I2 h RAh [13] Hour of Right Ascension (J2000) 10- 11 I2 min RAm [36/37] Minute of Right Ascension (J2000) 13- 17 F5.2 s RAs Second of Right Ascension (J2000) 19 A1 --- DE- [-] Sign of the Declination (J2000) 20- 21 I2 deg DEd [29] Degree of Declination (J2000) 23- 24 I2 arcmin DEm [46/59] Arcminute of Declination (J2000) 26- 29 F4.1 arcsec DEs Arcsecond of Declination (J2000) 31- 34 F4.1 kpc Rad [0.1/12] Galactic radius 36- 38 F3.1 arcsec Diam [0.8/6] Diameter of circular regions used for flux extractions (3) 40- 44 F5.1 10-19W/m2 F(Ha) [0.3/236] Hα flux (4) 46- 49 F4.1 10-19W/m2 F([SII]) [0/83] Flux of [SII] (4) 51- 55 F5.1 10-19W/m2 F([OIII]) [0/185] Flux of [OIII] (4) 57- 60 F4.2 --- [SII]/Ha [0/2] Ratio of [SII] to Hα 62- 65 F4.2 --- [OIII]/Ha [0/6] Ratio of [OIII] to Hα 67 A1 --- X [y/n] X-ray? (5) 69- 90 A22 --- OName Other names (6)
Note (1): Numbering in table 3 begins at 301 to separate this group from the ISM SNR sample (table 2). Note (2): x = Position and size for object 014 has been slightly revised since the original paper (J/ApJS/203/8). Note (3): Diameter of the circular regions used for flux extractions; these are effectively upper limits for the object sizes. Note (4): In units of 10-16erg/cm2/s; a correction factor of 1.45 has been applied to Hα (see the text). Note (5): A "y" indicates a likely X-ray detection in deep Chandra data (Long+ 2014, J/ApJS/212/21). Note (6): Other Name abbreviations: BL = Blair & Long (2004ApJS..155..101B; <[BL2004b] SNR NN> in Simbad); SW = Soria & Wu (2003, Cat. J/A+A/410/53; <[SW2003] NNN> in Simbad); H = Hadfield et al. (2005, Cat. J/A+A/439/265; <[HCS2005] NNN> for Simbad); D10 = Dopita et al. (2010ApJ...710..964D) D10-T4 = Table 4, Dopita et al. (2010ApJ...710..964D); L = Long el al. (2014, J/ApJS/212/21).
History: From electronic version of the journal 21-Jan-2013: Insert into VizieR 28-Aug-2017: Updated versions of tables 2 and 3 from erratum published in 2017, ApJS, 229, 43
(End) Emmanuelle Perret [CDS] 04-Dec-2012
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