The luminosity function and the rate of Swift's Gamma Ray Bursts

By D. Wanderman, T. Piran. 2009

283 citations recorded by the source corpus.

We invert directly the redshift-luminosity distribution of observed long Swift gamma-ray bursts (GRBs) to obtain their rate and luminosity function. Our best-fitting rate is described by a broken power law that rises like (1 + 2) 2.1+0.5 -0.6 for 0 3. The local rate is ρ 0 ≃ 1.3 +0.6 -0.7 (Gpc -3 yr -1 ). The luminosity function is well described by a broken power law with a break at L* ≃ 10 52.5±0.2 (erg s -1 ) and with indices α = 0.2 +0.2 -0.1 and β = 1.4 +0.3 -0.6 . The recently detected GRB 090423, with z ≈ 8, fits nicely into the model's prediction, verifying that we are allowed to extend our results to high redshifts. While the GRB rate may follow the star formation rate (SFR) for z < 3, the high-redshift slope is shallower than the steep decline in the SFR for 4 < z. However, we cannot rule out a GRB rate that follows one of the recent SFR models.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/1b6a979f335598c379f5c2b30458bec10b464a41

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In Astronomy and Astrophysics

1. Bing Zhang
2. B. Metzger
3. E. Berger
4. Pawan Kumar
5. E. Nakar
6. T. Piran
7. E. Quataert
8. B. Margalit

Citations in the corpus

• CONNECTING THE GAMMA RAY BURST RATE AND THE COSMIC STAR FORMATION HISTORY: IMPLICATIONS FOR REIONIZATION AND GALAXY EVOLUTION (2011, background): “In other words, the decline in the GRB rate at z > 4 is considerably less rapid than the decrease in the star formation rate (e.g., Wanderman & Piran 2010).”
• THE OBSERVABLE SIGNATURES OF GRB COCOONS (2016, methodology): “We take RGRBs ≈ 1Gpc−3yr−1 as the local rate of observed LGRBs, i.e., GRBs with jet that points towards us (e.g., Wanderman & Piran 2010).”
• The Zwicky Transient Facility Bright Transient Survey. II. A Public Statistical Sample for Exploring Supernova Demographics (2020, methodology): “The GRB rate is consistent with expectations given the on-axis GRB rate of ∼1 Gpc−3 yr−1 (Wanderman & Piran 2010), assuming we would only be sensitive to events seen within a viewing angle of θ<3θjet at this luminosity threshold.”
• Millisecond Magnetar Birth Connects FRB 121102 to Superluminous Supernovae and Long-duration Gamma-Ray Bursts (2017, methodology): “This is comparable to the estimated beaming-correct local (z ≈ 0) rate of LGRBs of ≈ 130+60−70 Gpc−3 yr−1 for an assumed beaming fraction of fb = 1/100 (Wanderman & Piran 2010).”
• The physics of gamma-ray bursts & relativistic jets (2014, background): “Several studies agree that the high-luminosity slope is steep: α2 ∼ 2.5 (e.g. Liang et al., 2007a; Virgili et al., 2009; Wanderman and Piran, 2010).”
• The rate, luminosity function and time delay of non-Collapsar short GRBs (2014, methodology): “When comparing the luminosity function found here for sGRBs with the long GRBs luminosity function (Wanderman & Piran 2010) we find that the break luminosity is close (L∗sGRB = 2 × 1052 and L∗LGRB = 3 × 1052), but the sGRB luminosity function is steeper compared with the LGRB luminosity function…”
• Stellar black holes at the dawn of the universe (2011, background): “There is increasing evidence for an enhanced LGRB rate at z > 3 (Daigne et al. 2006; Kistler et al. 2008; Wanderman & Piran 2010; Qin et al. 2010), as expected from the increase in the specific star formation rate (SFR) with decreasing metallicity (Mannucci et al. 2010).”