scholarly journals A method for quantifying the gamma-ray burst bias. Application in the redshift range of 0–1.1

2013 ◽  
Vol 557 ◽  
pp. A34 ◽  
Author(s):  
S. Boissier ◽  
R. Salvaterra ◽  
E. Le Floc’h ◽  
S. Basa ◽  
V. Buat ◽  
...  
Keyword(s):  
Gamma Ray ◽  
Gamma Ray Burst ◽  
Redshift Range

scholarly journals What is the Real Shape of the Hubble Diagram, z = H0*D or z+1= eH0*t? Analysis of the SN1a Supernovae and Gamma Ray Burst Redshift/Magnitude Data including the High Redshift Range up to z = 8.1

2020 ◽  
Author(s):  
Laszlo Marosi
Keyword(s):  
Gamma Ray ◽  
High Redshift ◽  
Flight Time ◽  
Gamma Ray Bursts ◽  
Hubble Diagram ◽  
Gamma Ray Burst ◽  
Redshift Range ◽  
The Real

Analyses of the Hubble diagrams are presented for SN1a supernovae and gamma ray bursts in the redshift ranges z = 0.01–1.3 and 0.034–8.1, respectively. Data are presented on the typical z/μ scale and also on the less common yet increasingly sensitive photon flight time t/(z+1) scale. The primary conclusion is that on the basis of the presently accessible data in the redshift range z = 0.01–8.1, the slope of the Hubble diagram is, or is extremely close to, exponential.

scholarly journals Cosmology and the Subgroups of Gamma-ray Bursts

10.14311/1330 ◽  
2011 ◽  
Vol 51 (1) ◽  
Author(s):  
A. Mészáros ◽  
J. Řípa ◽  
L. G. Balázs ◽  
Z. Bagoly ◽  
P. Veres ◽  
...  
Keyword(s):  
Gamma Ray ◽  
Gamma Ray Bursts ◽  
Gamma Ray Burst ◽  
Redshift Range ◽  
Cosmological Principle

Both short and intermediate gamma-ray bursts are distributed anisotropically in the sky (Mészáros, A. et al. ApJ, 539, 98 (2000), Vavrek, R. et al. MNRAS, 391, 1 741 (2008)). Hence, in the redshift range, where these bursts take place, the cosmological principle is in doubt. It has already been noted that short bursts should be mainly at redshifts smaller than one (Mészáros, A. et al. Gamma-ray burst: Sixth Huntsville Symp., AIP, Vol. 1 133, 483 (2009); Mészáros, A. et al. Baltic Astron., 18, 293 (2009)). Here we show that intermediate bursts should be at redshifts up to three.

scholarly journals Magnetohydrodynamic simulations of gamma-ray burst jets: Beyond the progenitor star

New Astronomy ◽  
2010 ◽  
Vol 15 (8) ◽  
pp. 749-754 ◽  
Author(s):  
Alexander Tchekhovskoy ◽  
Ramesh Narayan ◽  
Jonathan C. McKinney
Keyword(s):  
Gamma Ray ◽  
Gamma Ray Burst ◽  
Magnetohydrodynamic Simulations

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).

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