2018A&A...616A..98S


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.14CEST19:11:22

2018A&A...616A..98S - Astronomy and Astrophysics, volume 616A, 98-98 (2018/8-1)

G51.04+0.07 and its environment: Identification of a new Galactic supernova remnant at low radio frequencies.

SUPAN L., CASTELLETTI G., PETERS W.M. and KASSIM N.E.

Abstract (from CDS):

We have identified a new supernova remnant (SNR), G51.04+0.07, using observations at 74 MHz from the Very Large Array Low-Frequency Sky Survey Redux (VLSSr). Earlier, higher frequency radio continuum, recombination line, and infrared data had correctly inferred the presence of nonthermal radio emission within a larger, complex environment including ionised nebulae and active star formation. However, our observations have allowed us to redefine at least one SNR as a relatively small source (7.5'x3' in size) located at the southern periphery of the originally defined SNR candidate G51.21+0.11. The integrated flux density of G51.04+0.07 at 74MHz is 6.1±0.8Jy, while its radio continuum spectrum has a slope α=-0.52±0.05 (Sv∝vα), typical of a shell-type remnant. We also measured spatial variations in the spectral index between 74 and 1400MHz across the source, ranging from a steeper spectrum (α=-0.50±0.04) coincident with the brightest emission to a flatter component (α=-0.30±0.07) in the surrounding fainter region. To probe the interstellar medium into which the redefined SNR is likely evolving, we have analysed the surrounding atomic and molecular gas using the 21cm neutral hydrogen (HI) and 13CO (J=1-0) emissions. We found that G51.04+0.07 is confined within an elongated HI cavity and that its radio emission is consistent with the remains of a stellar explosion that occurred ∼6300yr ago at a distance of 7.7±2.3kpc. Kinematic data suggest that the newly discovered SNR lies in front of HII regions in the complex, consistent with the lack of a turnover in the low frequency continuum spectrum. The CO observations revealed molecular material that traces the central and northern parts of G51.04+0.07. The interaction between the cloud and the radio source is not conclusive and motivates further study. The relatively low flux density (∼1.5Jy at 1400MHz) of G51.04+0.07 is consistent with this and many similar SNRs lying hidden along complex lines of sight towards inner Galactic emission complexes. It would also not be surprising if the larger complex studied here hosted additional SNRs.

Abstract Copyright: © ESO 2018

Journal keyword(s): ISM: supernova remnants - ISM: individual objects: G51.04+0.07 - radio continuum: general

Simbad objects: 13

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Number of rows : 13

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 IC 443 SNR 06 18 02.7 +22 39 36           ~ 1101 1
2 SNR G015.4+00.1 Rad 18 18.0 -15 27           ~ 24 1
3 3C 391.0 Rad 18 49 23.3 -00 55 38           ~ 319 2
4 SNR G039.2-00.3 SNR 19 04 04.50 +05 27 12.0           ~ 172 1
5 3C 397 SNR 19 07 33.20 +07 08 32.0           ~ 191 2
6 W 49b SNR 19 11 09.000 +09 06 24.00           ~ 394 1
7 [LPH96] 050.857+0.081 HII 19 24 42.2 +15 56 08           ~ 3 0
8 [KB94] 67 HII 19 24 48.4 +16 09 10           ~ 6 0
9 SNR G051.04+00.07 SNR 19 25.1 +16 05           ~ 2 0
10 SNR G051.21+00.11 SR? 19 25 17 +16 15.6           ~ 4 0
11 FL8Y J1925.4+1616 gam 19 25.4 +16 16           ~ 1 0
12 PSR J1926+1613 Psr 19 26.0 +16 13           ~ 3 0
13 [KB94] 68 HII 19 26 00.1 +16 20 29           ~ 4 0

    Equat.    Gal    SGal    Ecl

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2020.07.14-19:11:22

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