CDS

2016A&A...595A..72M

Query : 2016A&A...595A..72M

2016A&A...595A..72M - Astronomy and Astrophysics, volume 595A, 72-72 (2016/11-1)

GRB 980425 host: [C II], [O I], and CO lines reveal recent enhancement of star formation due to atomic gas inflow.

MICHALOWSKI M.J., CASTRO CERON J.M., WARDLOW J.L., KARSKA A., MESSIAS H., VAN DER WERF P., HUNT L.K., BAES M., CASTRO-TIRADO A.J., GENTILE G., HJORTH J., LE FLOC'H E., PEREZ-MARTINEZ R., NICUESA GUELBENZU A., RASMUSSEN J., RIZZO J.R., ROSSI A., SANCHEZ-PORTAL M., SCHADY P., SOLLERMAN J. and XU D.

Abstract (from CDS):

Context. Accretion of gas from the intergalactic medium is required to fuel star formation in galaxies. We have recently suggested that this process can be studied using host galaxies of gamma-ray bursts (GRBs).
Aims. Our aim is to test this possibility by studying in detail the properties of gas in the closest galaxy hosting a GRB (980425).
Methods. We obtained the first ever far-infrared (FIR) line observations of a GRB host, namely Herschel/PACS resolved [CII] 158µm and [OI] 63µm spectroscopy, and an APEX/SHeFI CO(2-1) line detection and ALMA CO(1-0) observations of the GRB 980425 host.
Results. The GRB 980425 host has elevated [CII]/FIR and [OI]/FIR ratios and higher values of star formation rates (SFR) derived from line ([CII], [OI], Hα) than from continuum (UV,IR, radio) indicators. [CII] emission exhibits a normal morphology, peaking at the galaxy centre, whereas [OI] is concentrated close to the GRB position and the nearby Wolf-Rayet region. The high [OI] flux indicates that there is high radiation field and high gas density at these positions, as derived from modelling of photo-dissociation regions. The [CII]/CO luminosity ratio of the GRB 980425 host is close to the highest values found for local star-forming galaxies.Indeed, its CO-derived molecular gas mass is low given its SFR and metallicity, but the [CII]-derived molecular gas mass is close to the expected value.
Conclusions. The [OI] and HI concentrations and the high radiation field and density close to the GRB position are consistent with the hypothesis of a very recent (at most a few tens of Myr ago) inflow of atomic gas triggering star formation.In this scenario dust has not had time to build up (explaining high line-to-continuum ratios). Such a recent enhancement of star formation activity would indeed manifest itself in high SFRline/SFRcontinuum ratios because the line indicators are sensitive only to recent (≤10Myr) activity, whereas the continuum indicators measure the SFR averaged over much longer periods (∼100Myr). Within a sample of 32 other GRB hosts, 20 exhibit SFRline/SFRcontinuum>1 with a mean ratio of 1.74±0.32. This is consistent with a very recent enhancement of star formation that is common among GRB hosts, so galaxies that have recently experienced inflow of gas may preferentially host stars exploding as GRBs. Therefore GRBs may be used to select a unique sample of galaxies that is suitable for the investigation of recent gas accretion.

Abstract Copyright: © ESO, 2016

Journal keyword(s): dust, extinction - galaxies: individual: ESO 184-G82 - galaxies: ISM - galaxies: star formation - submillimeter: galaxies - gamma-ray burst: individual: 980425

CDS comments: Calibrator J1945-552 not identified.

Simbad objects: 65

goto Full paper

goto View the references in ADS

Number of rows : 65
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023 		#notes
1 [SKP2006] GRB 041006 Host G G 00 54 50.17 +01 14 07.0           ~ 5 0
2 GRB 041006 gB 00 54 50.17 +01 14 07.0           ~ 195 2
3 GRB 000210 gB 01 59 15 -40 40.0           ~ 170 0
4 [LDM2003] GRB J015915.5-403933 G 01 59 15.61 -40 39 33.1           ~ 13 0
5 GRB 040924 gB 02 06 22.52 +16 08 48.8           ~ 160 1
6 [WSR2004] Host G G 02 06 22.52 +16 08 48.8           ~ 7 1
7 [PBK2002] GRB 000911 Host Galaxy G 02 18 34.360 +07 44 27.65           ~ 7 0
8 GRB 000911 gB 02 18 42 +07 48.0           ~ 154 0
9 SN 2006aj SN* 03 21 39.670 +16 52 02.27 17.96 19.11 17.40     SNIc-BL 919 1
10 2XMM J032139.6+165202 G 03 21 39.693 +16 52 01.74           ~ 18 1
11 GRB 970228 gB 05 01 46.7 +11 46 53           ~ 636 1
12 [LDM2003] GRB J050146.7+114654 G 05 01 46.7 +11 46 54           ~ 10 1
13 GRB 990705 gB 05 09 54.5 -72 07 53           ~ 222 1
14 [LDM2002] J050954.8-720754 G 05 09 54.8 -72 07 54           ~ 15 1
15 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 16973 1
16 RMC 136 Cl* 05 38 42.396 -69 06 03.36           ~ 1955 1
17 [RWP2006] J054624.428+641238.78 G 05 46 24.428 +64 12 38.78           ~ 3 1
18 GRB 061126 gB 05 46 24.460 +64 12 38.49 18.62 18.79 19.20     ~ 171 1
19 GRB 050826 gB 05 51 01.590 -02 38 35.40           ~ 122 0
20 GRB 970508 gB 06 53 49.2 +79 16 19           ~ 864 1
21 [LDM2003] GRB J065349.4+791619 G 06 53 49.4 +79 16 19           ~ 10 1
22 SN 2003lw SN* 08 02 30.1 -39 51 03       20.23   SNIc: 535 0
23 Anon J080230-3951 G 08 02 30.20 -39 51 03.0 22.31 22.32 20.53 20.44 19.40 ~ 20 0
24 GRB 070306 gB 09 52 23.220 +10 28 55.20           ~ 201 1
25 SDSS J095223.31+102855.4 G 09 52 23.32 +10 28 55.4       23.00   ~ 7 0
26 [HTN2002] A G 10 17 44 +71 29.9           ~ 13 1
27 GRB 980613 gB 10 17 57.8 +71 27 26           ~ 201 1
28 SN 2003dh SN* 10 44 50.030 +21 31 18.15     16.2     SNIcpec 1193 1
29 GRB 011121 gB 11 34 26.67 -76 01 41.6       23.0   ~ 270 1
30 Anon J113429-7601 G 11 34 29.88 -76 01 41.6           ~ 9 0
31 GRB 990506 gB 11 54 41 -26 45.0           ~ 165 1
32 [LDM2003] GRB J115450.1-264035 G 11 54 50.1 -26 40 35           ~ 10 1
33 [BCK2003] G1 G 12 25 19.3 +20 06 11           ~ 19 0
34 GRB 000418 gB 12 25 21 +20 05.0           ~ 212 0
35 [MPP2003] GRB 020405 abs 0.6908 G 13 58 03.01 -31 22 24.7           ~ 7 1
36 GRB 020405 gB 13 58 03.12 -31 22 22.2   21.9 21.5     ~ 246 1
37 [LDM2003] GRB J163353.5+462721 G 16 33 53.5 +46 27 21           ~ 10 1
38 GRB 991208 gB 16 33 53.51 +46 27 21.5           ~ 256 1
39 GRB 030528 gB 17 04 00.3 -22 37 10           ~ 88 1
40 [RSG2005] GRB 030528 Host G G 17 04 02 -22 39.0           ~ 4 1
41 QSO B1730-130 QSO 17 33 02.70578907 -13 04 49.5482119   18 19.50 18.78 17.39 ~ 1107 1
42 GRB 050223 gB 18 05 32.200 -62 28 20.40           ~ 105 0
43 [PDL2006] H G 18 05 32.992 -62 28 18.81           ~ 3 0
44 GRB 970828 gB 18 08 31.6 +59 18 51           ~ 345 1
45 [LDM2003] GRB J180831.6+591851 G 18 08 31.6 +59 18 51           ~ 14 1
46 [TSC98] Host G G 19 34 54 -52 49.9           ~ 20 1
47 SN 1998bw SN* 19 35 03.17 -52 50 46.1   14.09       SNIc 1794 2
48 ESO 184-82 G 19 35 04.416 -52 50 38.04   15.17   14.26   ~ 106 2
49 GRB 020813A gB 19 46 41.874 -19 36 04.81           ~ 301 0
50 [PBF2006d] Host Galaxy G 21 23 27.0 -53 02 02           ~ 15 1
51 GRB 060614 gB 21 23 32.140 -53 01 36.10 18.89 20.12 19.54     ~ 582 1
52 GRB 060505 gB 22 07 03.440 -27 48 51.89           ~ 252 1
53 2dFGRS TGS173Z112 G 22 07 03.5 -27 48 57 18.43 18.89 18.27 17.90 17.51 ~ 18 1
54 GRB 990712 gB 22 31 53.061 -73 24 28.58           ~ 259 1
55 [LDM2003] GRB J223153.1-732429 G 22 31 53.1 -73 24 29           ~ 14 1
56 APMUKS (BJ) B224600.67-210204.6 G 22 48 42.3391 -20 46 08.945   20.7 20.8     ~ 12 1
57 GRB 020903 gB 22 48 42.34 -20 46 09.3           ~ 230 1
58 GRB 010921 gB 22 55 59.90 +40 55 52.9           ~ 169 1
59 [LDM2003] GRB J225559.9+405553 G 22 55 59.9 +40 55 53           ~ 12 1
60 GRB 020819 gB 23 00 12 -43 00.7           ~ 128 1
61 [FB2003] J232719.475+061555.95 G 23 27 19.475 +06 15 55.95           ~ 11 1
62 [CDB2005b] B G 23 56 04.10 +19 36 24.2           ~ 12 1
63 GRB 051022A gB 23 56 04.200 +19 36 32.30           ~ 180 1
64 [LDM2003] GRB J235906.7+083507 G 23 59 06.7 +08 35 07   23.04 23.02     ~ 23 1
65 GRB 980703 gB 23 59 06.7 +08 35 07           ~ 442 1

To bookmark this query, right click on this link: simbad:objects in 2016A&A...595A..72M and select 'bookmark this link' or equivalent in the popup menu

2023.09.23-16:57:56

© Université de Strasbourg/CNRS

    • Contact