2009A&A...503..783S


C.D.S. - SIMBAD4 rel 1.7 - 2020.01.26CET01:00:54

2009A&A...503..783S - Astronomy and Astrophysics, volume 503, 783-795 (2009/9-1)

A multiwavelength study of Swift GRB 060111B constraining the origin of its prompt optical emission.

STRATTA G., POZANENKO A., ATTEIA J.-L., KLOTZ A., BASA S., GENDRE B., VERRECCHIA F., BOEER M., CUTINI S., HENZE M., HOLLAND S., IBRAHIMOV M., IENNA F., KHAMITOV I., KLOSE S., RUMYANTSEV V., BIRYUKOV V., SHARAPOV D., VACHIER F., ARNOUTS S. and PERLEY D.A.

Abstract (from CDS):

The detection of bright optical emission measured with good temporal resolution during the prompt phase of GRB 060111B makes this GRB a rare event that is especially useful for constraining theories of the prompt emission. For this reason an extended multi-wavelength campaign was performed to further constrain the physical interpretation of the observations. In this work, we present the results obtained from our multi-wavelength campaign, as well as from the public Swift/BAT, XRT, and UVOT data. We identified the host galaxy at R∼25mag from deep R-band exposures taken 5 months after the trigger. Its featureless spectrum and brightness, as well as the non-detection of any associated supernova 16 days after the trigger, enabled us to constrain the distance scale of GRB 060111Bwithin 0.4≤z≤3 in the most conservative case. The host galaxy spectral continuum is best fit with a redshift of z∼2, and other independent estimates converge to z∼1-2. From the analysis of the early afterglow SED, we find that non-negligible host galaxy dust extinction, in addition to the Galactic one, affects the observed flux in the optical regime. The extinction-corrected optical-to-gamma-ray SED during the prompt emission shows a flux density ratio Fγ/Fopt=10–2-10–4 with spectral index βγ,optγ, strongly suggesting a separate origin of the optical and gamma-ray components. This result is supported by the lack of correlated behavior in the prompt emission light curves observed in the two energy domains. The temporal properties of the prompt optical emission observed during GRB 060111B and their similarities to other rapidly-observed events favor interpretation of this optical light as radiation from the reverse shock. Observations are in good agreement with theoretical expectations for a thick shell limit in slow cooling regime. The expected peak flux is consistent with the observed one corrected for the host extinction, likely indicating that the starting time of the TAROT observations is very near to or coincident with the peak time. The estimated fireball initial Lorentz factor is Γ≥260-360 at z=1-2, similar to the Lorentz factors obtained from other GRBs. GRB 060111Bis a rare case of a GRB with both a bright, well-observed optical counterpart and a ``canonical'' early X-ray light curve, thus providing a good test case of the reverse shock emission mechanism in both energy ranges.

Abstract Copyright:

Journal keyword(s): gamma rays: bursts - radiation mechanisms: non-thermal - methods: data analysis

Nomenclature: Text: [SPA2009] GRB 060111B Host G N=1. Paragr. 4.3: [SPA2009] JHHMMSS.ss+DDMMSS.s N=1.

Simbad objects: 12

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Number of rows : 12

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 NAME SMC G 00 52 38.0 -72 48 01   2.79 2.2     ~ 9184 1
2 GRB 061126 gB 05 46 24.460 +64 12 38.49 18.62 18.79 19.20     ~ 148 1
3 SN 2002lt SN* 08 08 59.858 +06 43 37.52           SN.Ic:(~) 334 1
4 GRB 090102 gB 08 32 59.50 +33 06 25.7           ~ 175 0
5 SN 1994I SN* 13 29 54.072 +47 11 30.50     12.9     SNIc 561 1
6 GRB 080319B gB 14 31 41.04 +36 18 09.2           ~ 417 0
7 GRB 990123 gB 15 25 29 +44 45.0     8.95     ~ 957 1
8 GRB 060111B gB 19 05 42.480 +70 22 33.60     17.55     ~ 79 1
9 [SPA2009] GRB 060111B Host G G 19 05 42.75 +70 22 33.3           ~ 1 0
10 [SPA2009] J190543.06+702229.7 G 19 05 43.1 +70 22 30           ~ 1 0
11 SN 1998bw SN* 19 35 03.17 -52 50 46.1   14.09       SNIc 1623 2
12 GRB 060117 gB 21 51 36.130 -59 58 39.10           ~ 54 0

    Equat.    Gal    SGal    Ecl

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