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J/ApJ/793/134            M33 SNR candidates properties              (Lee+, 2014)

Properties of optically selected supernova remnant candidates in M33. Lee J.H., Lee M.G. <Astrophys. J., 793, 134 (2014)> =2014ApJ...793..134L (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, nearby ; Supernova remnants ; Stars, diameters ; Photometry, H-alpha Keywords: galaxies: individual: M33 - galaxies: ISM - ISM: supernova remnants Abstract: Narrowband images covering strong emission lines are efficient for surveying supernova remnants (SNRs) in nearby galaxies. Using the narrowband images provided by the Local Group Galaxy Survey, we searched for SNRs in M33. Culling the objects with enhanced [S II]/Hα and round morphology in the continuum-subtracted Hα and [S II] images, we produced a list of 199 sources. Among them, 79 are previously unknown. Their progenitor and morphology types were classified. A majority of the sample (170 objects) are likely remnants of core-collapse supernovae (SNe), and 29 are remnants of Type Ia SNe. The cumulative size distribution of these objects is found to be similar to that of the M31 remnants derived in a similar way. We obtain a power-law slope, α=2.38±0.05. Thus, a majority of the sources are considered to be in the Sedov-Taylor phase, consistent with previous findings. The histogram of the emission-line ratio ([S II]/Hα) of the remnants has two concentrations at [S II]/Hα ∼0.55 and ∼0.8, as in M31. Interestingly, LX(and L_20 cm_) of the compact center-bright objects are correlated with their optical luminosity. The remnants with X-ray emission have brighter optical surface brightnesses and smaller diameters than those without X-ray emission. Description: We utilized the Hα and [S II] images in the LGGS to find new M33 remnants. The LGGS covered three 36' square fields of M33. We subtracted continuum sources from the narrowband images using R-band images. We smoothed the images with better seeing to match the point-spread function in the images with worse seeing, using the IRAF task psfmatch. We then scaled and subtracted the resulting continuum images from narrowband images. We selected M33 remnants considering three criteria: emission-line ratio ([S II]/Hα), the morphological structure, and the absence of blue stars inside the sources. Details are described in L14 (Lee et al. 2014ApJ...786..130L). We detected objects with [S II]/Hα>0.4 in emission-line ratio maps, and selected objects with round or shell structures in each narrowband image. As a result, we chose 435 sources. Objects: ---------------------------------------------------------- RA (ICRS) DE Designation(s) ---------------------------------------------------------- 01 33 50.90 +30 39 35.8 M33 = NGC 598 ---------------------------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 51 17 A List of Previous M33 SNR Candidates Excluded in This Study table3.dat 63 199 A List of M33 SNR Candidates
See also: VII/272 : A catalogue of Galactic supernova remnants (Green, 2014) J/ApJ/703/370 : Radio SNRs in nearby galaxies (Chomiuk+, 2009) J/ApJS/187/495 : SNRs in M33 from optical and X-ray (Long+, 2010) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 4 A4 --- --- [L10-] 5- 7 A3 --- Name Source identifier ([LBW2010] NNN in Simbad) (G3) 9- 18 F10.7 deg RAdeg Right Ascension in decimal degrees (J2000) (G1) 20- 28 F9.6 deg DEdeg Declination in decimal degrees (J2000) (G1) 30- 34 F5.2 [10-7W] logLHa Log of Hα luminosity; erg/s (G2) 36- 40 F5.2 [10-7W] logLSII Log of [S II] luminosity; erg/s (G2) 42- 44 I3 pc Diam Diameter calculated using 1''=3.88 pc 46- 49 F4.2 --- Ratio Ratio of [S II] to Hα 51 A1 --- Class [HS] Classification (3)
Note (3): Class as follows: H = H II regions with [S II]:Hα<0.4, and blue stars inside; S = Superbubbles (Larger than D=100 pc and a number of blue stars inside).
Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 3 I3 --- ID [1/199] Index number 5- 14 F10.7 deg RAdeg Right Ascension in decimal degrees (J2000) (G1) 16- 24 F9.6 deg DEdeg Declination in decimal degrees (J2000) (G1) 26- 30 F5.2 [10-7W] logLHa Log of Hα luminosity; erg/s (G2) 32- 36 F5.2 [10-7W] logLSII Log of [S II] luminosity; erg/s (G2) 38- 40 I3 pc Diam Diameter calculated using 1''=3.88 pc (3) 42- 45 F4.2 --- Ratio Ratio of [S II] to Hα 47- 48 A2 --- Morph Morphology type (C,A1,A2,A3,B1,B2,B3) 50- 52 I3 --- N(OB) Number of OB stars (4) 54- 55 A2 --- PType Progenitor type (CC,Ia) 57- 63 A7 --- Com Comments (G3)
Note (3): For d=800 kpc. Note (4): Located between the boundary of each SNR candidate and 100 pc from the center of each SNR candidate.
Global notes: Note (G1): Measured in the Hα image. Note (G2): Calculated using L=4πd2*flux for d=800kpc. Note (G3): L10 identifier coming from Long et al. (2010, J/ApJS/187/495)
History: From electronic version of the journal
(End) Prepared by [AAS], Tiphaine Pouvreau [CDS] 20-Apr-2017
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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