2024ApJ...971L..51B

Query : 2024ApJ...971L..51B

2024ApJ...971L..51B - Astrophys. J., 971, L51 (2024/August-3)

Host Galaxies for Four Nearby CHIME/FRB Sources and the Local Universe FRB Host Galaxy Population.

BHARDWAJ M., MICHILLI D., KIRICHENKO A.Y., MODILIM O., SHIN K., KASPI V.M., ANDERSEN B.C., CASSANELLI T., BRAR C., CHATTERJEE S., COOK A.M., DONG F.A., FONSECA E., GAENSLER B.M., IBIK A.L., KACZMAREK J.F., LANMAN A.E., LEUNG C., MASUI K.W., PANDHI A., PEARLMAN A.B., PETROFF E., PLEUNIS Z., PROCHASKA J.X., RAFIEI-RAVANDI M., SAND K.R., SCHOLZ P. and SMITH K.M.

Abstract (from CDS):

We present the host galaxies of four apparently nonrepeating fast radio bursts (FRBs), FRB 20181223C, FRB 20190418A, FRB 20191220A, and FRB 20190425A, reported in the first Canadian Hydrogen Intensity Mapping Experiment (CHIME/FRB) catalog. Our selection of these FRBs is based on a planned hypothesis testing framework where we search all CHIME/FRB Catalog-1 events that have low extragalactic dispersion measure (<100 pc cm–3), with high Galactic latitude (∣b∣ > 10°) and saved baseband data. We associate the selected FRBs with galaxies with moderate to high star formation rates located at redshifts between 0.027 and 0.071. We also search for possible multimessenger counterparts, including persistent compact radio and gravitational-wave sources, and find none. Utilizing the four FRB hosts from this study, along with the hosts of 14 published local Universe FRBs (z < 0.1) with robust host association, we conduct an FRB host demographics analysis. We find all 18 local Universe FRB hosts in our sample to be spirals (or late-type galaxies), including the host of FRB 20220509G, which was previously reported to be elliptical. Using this observation, we scrutinize proposed FRB source formation channels and argue that core-collapse supernovae are likely the dominant channel to form FRB sources. Moreover, we infer no significant difference in the host properties of repeating and apparently nonrepeating FRBs in our local Universe FRB host sample. Finally, we find the burst rates of these four apparently nonrepeating FRBs to be consistent with those of the sample of localized repeating FRBs observed by CHIME/FRB. Therefore, we encourage further monitoring of these FRBs with more sensitive radio telescopes.

Abstract Copyright: © 2024. The Author(s). Published by the American Astronomical Society.

Journal keyword(s): Radio transient sources - Supernovae - Spiral galaxies - Neutron stars - Pulsars - Radio bursts - Transient sources

Simbad objects: 49

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Number of rows : 49
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 FRB 20200223B rB 00 28 16.800 +29 00 36.00           ~ 25 0
2 LEDA 1847306 G 00 33 04.68158 +28 49 52.6063           ~ 6 0
3 SDSS J015800.28+654253.0 G 01 58 00.28512 +65 42 53.0964           ~ 17 0
4 FRB 20180916B rB 01 58 00.750 +65 43 00.30           ~ 457 0
5 2MASX J02084091+7102087 GiG 02 08 40.8598703712 +71 02 09.146975892           ~ 20 0
6 FRB 20220319D rB 02 08 42.700 +71 02 06.94           ~ 39 0
7 NAME FRB 180814.J0422+73 rB 04 22 44.0 +73 39 52           ~ 112 0
8 FRB 20190418A rB 04 23 09.6000 +16 02 24.000           ~ 25 0
9 SDSS J042314.96+160425.6 G 04 23 14.96057 +16 04 25.6014           ~ 2 0
10 BD+52 913 WD* 05 05 30.6180977592 +52 49 51.919301604 10.25 11.44 11.69 11.93 12.108 DA.8 1153 0
11 FRB 20201124A rB 05 07 57.600 +26 11 24.00           ~ 307 0
12 NAME FRB 20201124A Host Galaxy G 05 08 03.49512 +26 03 37.9008           ~ 24 0
13 FRB 20181119D rB 05 31 58.6980 +33 08 52.588           ~ 933 0
14 M 81 Sy2 09 55 33.1726556496 +69 03 55.062505368   7.89 6.94     ~ 4725 3
15 FRB 20200120E rB 09 57 56.7 +68 49 32           ~ 219 0
16 SDSS J102924.22+012139.2 G 10 29 24.2259364008 +01 21 39.201915708           ~ 5 0
17 FRB 211212 rB 10 30 40.700 +01 40 36.80           ~ 30 0
18 NAME FRB 181030.J1054+73 rB 10 33 24.0000 +73 47 24.000           ~ 79 0
19 NGC 3252 GiG 10 34 23.104 +73 45 53.92   14.2       ~ 83 0
20 Feige 34 HS* 10 39 36.7358839104 +43 06 09.212615280 9.613 10.91 11.14 11.319 11.464 sdOp 731 0
21 PSO J180.9168+27.5457 G 12 03 40.04 +27 32 44.5           ~ 1 0
22 SDSS J120340.98+273251.5 G 12 03 40.99075 +27 32 51.6256           ~ 9 0
23 PSO J180.9355+27.5489 G 12 03 44.53 +27 32 55.9           ~ 1 0
24 PSO J180.9446+27.5463 G 12 03 46.72 +27 32 46.9           ~ 1 0
25 FRB 20181223C rB 12 04 12.0000 +27 34 48.000           ~ 24 0
26 FRB 211127 rB 13 19 09.500 -18 49 28.40           ~ 32 0
27 6dFGS gJ131914.0-185017 G 13 19 13.97 -18 50 16.7   16.51   15.29   ~ 8 0
28 MCG+08-25-050 G 13 51 59.172 +48 07 29.02   18       ~ 13 0
29 FRB 20190303A G 13 51 59.77 +48 06 57.6           ~ 58 0
30 MCG+08-25-049 G 13 51 59.8703271600 +48 07 14.191682376   18       ~ 10 0
31 FRB 20190520B rB 16 02 04.270 -11 17 17.32           ~ 211 0
32 FRB 20190110C rB 16 27 55.2000 +41 25 12.000           ~ 36 0
33 2MASS J17012149-4932475 G 17 01 21.49560 -49 32 47.5980           ~ 3 0
34 FRB 20210405I rB 17 01 21.50 -49 32 42.8           ~ 17 0
35 UGC 10667 G 17 02 38.9915055144 +21 34 36.332343012   16.0       ~ 28 0
36 FRB 20190425A rB 17 02 41.0 +21 34 34           ~ 47 0
37 PSR J1841-0456 Psr 18 41 19.29 -04 56 11.4           ~ 296 1
38 FRB 20220509G rB 18 50 40.800 +70 14 37.80           ~ 37 0
39 NAME Sgr 1935+2154 * 19 34 55.68 +21 53 48.2           ~ 820 1
40 PSO J310.1977+72.8826 G 20 40 47.443058 +72 52 57.24941           ~ 3 0
41 FRB 20220207C rB 20 40 47.890 +72 52 56.38           ~ 29 0
42 FRB 171020 rB 22 15.0 -19 40           ~ 54 0
43 ESO 601-36 AG? 22 15 24.75 -19 35 07.0   15.58   14.97 15.3 ~ 20 0
44 2E 4673 HXB 23 01 08.14 +58 52 44.5           ~ 673 1
45 FRB 20181220A rB 23 04 26.4000 +48 25 48.000           ~ 26 0
46 FRB 20220912A rB 23 09 04.9 +48 42 25           ~ 126 0
47 PSO J348.6982+48.3421 G 23 14 47.563 +48 20 31.55           ~ 4 0
48 NVSS J231448+482039 Rad 23 14 48.38 +48 20 39.9           ~ 1 0
49 GRB 190425 GWE ~ ~           ~ 438 0

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