scholarly journals The Host Galaxies of Short GRBs as Probes of Their Progenitor Properties

Galaxies ◽  
2019 ◽  
Vol 7 (1) ◽  
pp. 30 ◽  
Author(s):  
Massimiliano De Pasquale
Keyword(s):  
Star Formation ◽  
Gamma Ray ◽  
Compact Object ◽  
Host Galaxies ◽  
Gamma Ray Burst ◽  
Star Forming ◽  
Be Star ◽  
Short Grbs

We present and discuss the properties of host galaxies of short Gamma-ray Burst (SGRBs). In particular, we examine those observations that contribute to the understanding of the progenitor systems of these explosions. Most SGRB hosts are found to be star forming objects, but an important fraction, ∼1/5, of all hosts are elliptical with negligible star formation. Short bursts often occur at very large off-sets from their hosts, in regions where there is little or no underlying host light. Such results have enabled the community to test and improve the models for the production of short GRBs. In particular, the data are in favour of the merger of compact object binaries, provided that the kick velocities from the birth site are a few tens of km/s, and merger times of ∼1 Gyr.

scholarly journals Statistical Properties of Gamma-Ray Burst Host Galaxies

2012 ◽  
Vol 8 (S292) ◽  
pp. 190-190
Author(s):  
J. M. Chen ◽  
L. W. Jia ◽  
E. W. Liang
Keyword(s):  
Gamma Ray ◽  
Formation Rate ◽  
Neutral Hydrogen ◽  
Statistical Properties ◽  
Host Galaxy ◽  
Host Galaxies ◽  
Gamma Ray Burst ◽  
Star Forming ◽  
Hydrogen Column Density ◽  
Linear Fit

AbstractGRBs are the most luminous events in the Universe. They are detectable from local to high-z universe and may serve as probes for high-z galaxies (e.g., Savaglio et al. 2009; Kewley & Dopita 2002). We compile the observations for 61 GRB host galaxies from literature. Their redshifts range from 0.0085 to 6.295. We present the statistical properties of the GRB host galaxies, including the stellar mass (M*), star-forming rate (SFR), metallicity (Z), extinction (AV), and neutral hydrogen column density (NH). We explore possible correlations among the properties of gamma-ray burst host galaxies and their cosmic evolution with observations of 61 GRB host galaxies. Our results are shown in Figure 1. A clear Z-M* relation is found in our sample, which is Z ~ M0.4. The host galaxies of local GRBs with detection of accompanied supernovae also share the same relation with high-z GRB host galaxies. A trend that a more massive host galaxy tends to have a higher star-formation rate is found. The best linear fit gives a tentative relation, i.e, SFR ~ M0.75. No any correlation is found between AV and NH. A GRB host galaxy at a higher redshift also tends to have a higher SFR. Even in the same redshift, the SFR may vary over three orders of magnitude. The metallicity of the GRB host galaxies is statistically higher than that of the QSO DLAs. The full version of our results please refer to Chen et al. (2012).

scholarly journals Low radio-derived star formation rates in z < 0.5 gamma-ray burst host galaxies

2010 ◽  
Vol 409 (1) ◽  
pp. L74-L78 ◽  
Author(s):  
Elizabeth R. Stanway ◽  
Luke J. M. Davies ◽  
Andrew J. Levan
Keyword(s):  
Star Formation ◽  
Gamma Ray ◽  
Host Galaxies ◽  
Gamma Ray Burst

scholarly journals A Submillimeter and Radio Survey of Gamma‐Ray Burst Host Galaxies: A Glimpse into the Future of Star Formation Studies

2003 ◽  
Vol 588 (1) ◽  
pp. 99-112 ◽  
Author(s):  
E. Berger ◽  
L. L. Cowie ◽  
S. R. Kulkarni ◽  
D. A. Frail ◽  
H. Aussel ◽  
...  
Keyword(s):  
Star Formation ◽  
Gamma Ray ◽  
Host Galaxies ◽  
Gamma Ray Burst ◽  
The Future ◽  
Radio Survey

scholarly journals GAMMA-RAY BURST HOST GALAXIES AND THE LINK TO STAR-FORMATION

2008 ◽  
Author(s):  
J. P. U. FYNBO ◽  
J. HJORTH ◽  
D. MALESANI ◽  
J. SOLLERMAN ◽  
D. WATSON ◽  
...  
Keyword(s):  
Star Formation ◽  
Gamma Ray ◽  
Host Galaxies ◽  
Gamma Ray Burst

scholarly journals Inflow of atomic gas fuelling star formation

2015 ◽  
Vol 11 (A29B) ◽  
pp. 229-230
Author(s):  
M. J. Michałowski ◽  
G. Gentile ◽  
J. Hjorth ◽  
M. R. Krumholz ◽  
N. R. Tanvir ◽  
...  
Keyword(s):  
Star Formation ◽  
Gamma Ray ◽  
Molecular Gas ◽  
Host Galaxies ◽  
Gas Reservoirs ◽  
Gamma Ray Burst ◽  
Gas Cooling ◽  
Low Metallicity ◽  
Atomic Gas ◽  
Compact Array

AbstractGamma-ray burst host galaxies are deficient in molecular gas, and show anomalous metal-poor regions close to GRB positions. Using recent Australia Telescope Compact Array (ATCA) Hi observations we show that they have substantial atomic gas reservoirs. This suggests that star formation in these galaxies may be fuelled by recent inflow of metal-poor atomic gas. While this process is debated, it can happen in low-metallicity gas near the onset of star formation because gas cooling (necessary for star formation) is faster than the Hi-to-H2 conversion.

scholarly journals GRB host galaxies: theoretical investigation

2011 ◽  
Vol 7 (S279) ◽  
pp. 353-354
Author(s):  
Jirong Mao
Keyword(s):  
Dark Matter ◽  
Star Formation ◽  
Galaxy Evolution ◽  
Gamma Ray ◽  
Dark Matter Halo ◽  
Host Galaxy ◽  
Host Galaxies ◽  
X Ray ◽  
Star Forming ◽  
Stellar Masses

AbstractLong gamma-ray bursts (GRBs) can be linked to the massive stars and their host galaxies are assumed to be the star-forming galaxies within small dark matter halos. We apply a galaxy evolution model, in which the star formation process inside the virialized dark matter halo at a given redshift is achieved. The star formation rates (SFRs) in the GRB host galaxies at different redshifts can be derived from our model. The related stellar masses, luminosities, and metalicities of these GRB host galaxies are estimated. We also calculate the X-ray and optical absorption of GRB afterglow emission. At higher redshift, the SFR of host galaxy is stronger, and the absorption in the X-ray and optical bands of GRB afterglow is stronger, when the dust and metal components are locally released, surrounding the GRB environment. These model predictions are compared with some observational data as well.

scholarly journals Metallicity of stars formed throughout the cosmic history based on the observational properties of star-forming galaxies

2019 ◽  
Vol 488 (4) ◽  
pp. 5300-5326 ◽  
Author(s):  
Martyna Chruslinska ◽  
Gijs Nelemans
Keyword(s):  
Star Formation ◽  
Stellar Evolution ◽  
Gamma Ray ◽  
Formation Rate ◽  
Compact Object ◽  
Mass Function ◽  
Star Formation History ◽  
Mass Relation ◽  
Star Forming ◽  
The Galaxy

ABSTRACT Metallicity is one of the crucial factors that determine stellar evolution. To characterize the properties of stellar populations one needs to know the fraction of stars forming at different metallicities. Knowing how this fraction evolves over time is necessary e.g. to estimate the rates of occurrence of any stellar evolution related phenomena (e.g. double compact object mergers, gamma-ray bursts). Such theoretical estimates can be confronted with observational limits to validate the assumptions about the evolution of the progenitor system leading to a certain transient. However, to perform the comparison correctly one needs to know the uncertainties related to the assumed star formation history and chemical evolution of the Universe. We combine the empirical scaling relations and other observational properties of the star-forming galaxies to construct the distribution of the cosmic star formation rate density at different metallicities and redshifts. We address the question of uncertainty of this distribution due to currently unresolved questions, such as the absolute metallicity scale, the flattening in the star formation−mass relation or the low-mass end of the galaxy mass function. We find that the fraction of stellar mass formed at metallicities &lt;10 per cent solar (&gt;solar) since z = 3 varies by ∼18 per cent (∼26 per cent) between the extreme cases considered in our study. This uncertainty stems primarily from the differences in the mass–metallicity relations obtained with different methods. We confront our results with the local core-collapse supernovae observations. Our model is publicly available.

scholarly journals The host galaxy of GRB 980425/SN1998bw: a collisional ring galaxy

2019 ◽  
Vol 485 (4) ◽  
pp. 5411-5422 ◽  
Author(s):  
M Arabsalmani ◽  
S Roychowdhury ◽  
T K Starkenburg ◽  
L Christensen ◽  
E Le Floc’h ◽  
...  
Keyword(s):  
Star Formation ◽  
Gamma Ray ◽  
Dwarf Galaxy ◽  
Formation Rate ◽  
Host Galaxy ◽  
Gamma Ray Burst ◽  
Star Forming ◽  
Star Forming Regions ◽  
Very Large Telescope ◽  
Companion Galaxy

ABSTRACT We report Giant Metrewave Radio Telescope (GMRT), Very Large Telescope (VLT), and Spitzer Space Telescope observations of ESO 184−G82, the host galaxy of GRB 980425/SN 1998bw, that yield evidence of a companion dwarf galaxy at a projected distance of 13 kpc. The companion, hereafter GALJ193510-524947, is a gas-rich, star-forming galaxy with a star formation rate of $\rm 0.004\, M_{\odot }\, yr^{-1}$, a gas mass of $10^{7.1\pm 0.1} \, \mathrm{M}_{\odot}$, and a stellar mass of $10^{7.0\pm 0.3} \, \mathrm{M}_{\odot}$. The interaction between ESO 184−G82 and GALJ193510-524947 is evident from the extended gaseous structure between the two galaxies in the GMRT H i 21 cm map. We find a ring of high column density H i gas, passing through the actively star-forming regions of ESO 184−G82 and the GRB location. This ring lends support to the picture in which ESO 184−G82 is interacting with GALJ193510-524947. The massive stars in GALJ193510-524947 have similar ages to those in star-forming regions in ESO 184−G82, also suggesting that the interaction may have triggered star formation in both galaxies. The gas and star formation properties of ESO 184−G82 favour a head-on collision with GALJ193510-524947 rather than a classical tidal interaction. We perform state-of-the-art simulations of dwarf–dwarf mergers and confirm that the observed properties of ESO 184−G82 can be reproduced by collision with a small companion galaxy. This is a very clear case of interaction in a gamma-ray burst host galaxy and of interaction-driven star formation giving rise to a gamma-ray burst in a dense environment.

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