2010A&A...516A..71M


Query : 2010A&A...516A..71M

2010A&A...516A..71M - Astronomy and Astrophysics, volume 516, A71-71 (2010/6-2)

Optical and near-infrared follow-up observations of four Fermi/LAT GRBs: redshifts, afterglows, energetics, and host galaxies.

McBREEN S., KRUEHLER T., RAU A., GREINER J., KANN D.A., SAVAGLIO S., AFONSO P., CLEMENS C., FILGAS R., KLOSE S., KUEPCUE YOLDAS A., OLIVARES E.F., ROSSI A., SZOKOLY G.P., UPDIKE A. and YOLDAS A.

Abstract (from CDS):

Fermi can measure the spectral properties of gamma-ray bursts over a very large energy range and is opening a new window on the prompt emission of these energetic events. Localizations by the instruments on Fermi in combination with follow-up by Swift provide accurate positions for observations at longer wavelengths leading to the determination of redshifts, the true energy budget, host galaxy properties and facilitate comparison with pre-Fermi bursts. Multi-wavelength follow-up observations were performed on the afterglows of four bursts with high energy emission detected by Fermi/LAT: GRB090323, GRB090328, GRB090510 and GRB090902B. They were obtained in the optical/near-infrared bands with GROND mounted at the MPG/ESO 2.2m telescope and additionally of GRB090323 in the optical with the 2m telescope in Tautenburg, Germany. Three of the events are classified as long bursts while GRB090510 is a well localized short GRB with GeV emission. In addition, host galaxies were detected for three of the four bursts. Spectroscopic follow-up was initiated with the VLT for GRB090328 and GRB090510. The afterglow observations in 7 bands are presented for all bursts and their host galaxies are investigated. Knowledge of the distance and the local dust extinction enables comparison of the afterglows of LAT-detected GRBs with the general sample. The spectroscopic redshifts of GRB090328 and GRB090510 were determined to be z=0.7354±0.0003 and z=0.903±0.001 and dust corrected star-formation rates of 4.8M/yr and 0.60M/yr were derived for their host galaxies, respectively. The afterglows of long bursts exhibit power-law decay indices (α) from less than 1 to ∼2.3 and spectral indices (βopt) values from 0.65 to ∼1.2 which are fairly standard for GRB afterglows. Constraints are placed on the jet half opening angles of ≲2.1° to >6.4°, which allows limits to be placed on the beaming corrected energies. These range from ≲5x1050 erg to the one of the highest values ever recorded, >2.2x1052erg for GRB 090902B, and are not consistent with a standard candle. The extremely energetic long Fermi bursts have optical afterglows which lie in the top half of the brightness distribution of all optical afterglows detected in the Swift era or even in the top 5% if incompleteness is considered. The properties of the host galaxies of these LAT detected bursts in terms of extinction, star formation rates and masses do not appear to differ from previous samples.

Abstract Copyright:

Journal keyword(s): gamma-ray burst: individual: GRB 090323 - gamma-ray burst: individual: GRB 090328 - gamma-ray burst: individual: GRB 090510 - gamma-ray burst: individual: GRB 090902B

Nomenclature: [MKR2010] GRB YYMMDD Host G N=3.

CDS comments: Paragraph 1. GRB 081214 is a misprint for GRB 081224. Paragraph 3. Sloan standard star SA 114-650 is not in Simbad.

Simbad objects: 29

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Number of rows : 29
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 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 10529 1
2 NAME Hubble Ultra Deep Field reg 03 32 39.0 -27 47 29           ~ 1532 0
3 Fermi bn091031500 gB 04 47 -57.5           ~ 29 0
4 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 16507 1
5 Fermi bn090328401 gB 06 02 39.69 -41 52 55.1           ~ 158 1
6 [MKR2010] GRB 090328 Host G G 06 02 39.69 -41 52 55.1           ~ 1 1
7 Fermi bn080916009 gB 07 59 23.24 -56 38 16.8           ~ 343 0
8 Fermi bn090423330 gB 09 55 33.19 +18 08 57.7           ~ 339 0
9 Fermi bn090626189 gB 11 20 -33.5           ~ 50 0
10 GRB 050509B gB 12 36 18.000 +29 01 24.00           ~ 300 1
11 GRB 090426 gB 12 36 19.49 +32 59 05.5           ~ 188 0
12 [MKR2010] GRB 090323 Host G G 12 42 50.28 +17 03 11.9           ~ 1 1
13 Fermi bn090323002 gB 12 42 50.28 +17 03 11.9           ~ 201 1
14 Fermi bn090217206 gB 13 40 -08.4           ~ 51 0
15 GRB 081224 gB 14 12 35.85 +74 11 59.5           ~ 26 0
16 Fermi bn080825593 gB 15 28.8 -04 54           ~ 64 0
17 CD-38 10980 WD* 16 23 33.8380498896 -39 13 46.161043572 9.916 10.885 11.029 10.936 10.841 DA2 469 0
18 GRB 050724 gB 16 24 44.400 -27 32 27.90     19.70     ~ 415 1
19 Fermi bn091003191 gB 16 46 04.680 +36 37 31.08           ~ 113 0
20 Fermi bn090902462 gB 17 39 45.26 +27 19 28.1           ~ 362 0
21 CD-44 12736 PM* 18 36 25.9502475648 -44 18 36.907592904   10.83 10.22     G0 205 0
22 SN 1998bw SN* 19 35 03.17 -52 50 46.1   14.09       SNIc 1764 2
23 Fermi bn100116897 gB 20 20 +14.4           ~ 35 0
24 GRB 080514B gB 21 31 22.61 +00 42 30.3           ~ 62 0
25 Fermi bn081024891 gB 21 31 36.00 +21 12 14.4           ~ 87 0
26 [MKR2010] GRB 090510 Host G G 22 14 12.56 -26 34 58.7           ~ 2 1
27 Fermi bn090510016 gB 22 14 12.60 -26 35 51.1           ~ 473 1
28 SA 114-750 * 22 41 44.7035499504 +01 12 36.369967860 11.512 11.879 11.916 11.889 11.906 B9 41 0
29 Fermi bn090926181 gB 23 33 36.18 -66 19 25.9           ~ 284 0

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2023.01.27-09:01:20

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