Soft Gamma-Ray Repeaters in Nearby Galaxies: Rate, Luminosity Function, and Fraction among Short Gamma-Ray Bursts

It was suggested that some of the short-duration gamma-ray bursts (GRBs) are giant flares of soft gamma-ray repeaters (SGRs) in nearby galaxies. To test this hypothesis, I have constructed a sample of 47 short GRBs, detected by the Interplanetary Network (IPN), for which the position is constrained by at least one annulus on the celestial sphere. For each burst, I have checked whether its IPN 3 σ error region coincides with the apparent disk of one of 316 bright, star-forming galaxies found within 20 Mpc. I find a single match of GRB 000420B with M74, which could, however, be due to a chance coincidence. I estimate the IPN efficiency as a function of fluence and derive the galaxy sample completeness. I find that assuming there is a cutoff in the observed energy distribution of SGR flares at ≤10^(47) ergs, the fraction of SGRs among short GRBs with fluence above ~10^(-5) ergs cm^(-2) is <16% (95% confidence). I estimate the number of active SGRs in each one of the galaxies in the sample, and combine it with the distances to these galaxies, the IPN efficiency, and the SGR flare energy distribution, to derive the rate of giant flares with energy above 4 × 10^(46) ergs. I find that the rate of such giant flares is about (0.4-5) × 10^(-4) yr^(-1) per SGR. This rate is marginally consistent with the observed Galactic rate. Comparison of the Galactic rate with the inferred extragalactic rate implies a gradual cutoff (or steepening) of the flare energy distribution at ≾3 × 10^(46) ergs (95% confidence). Using the Galactic SGR flare rate, I set a lower limit of 1% on the fraction of SGR flares among short GRBs

Calibrated griz magnitudes of Tycho stars: All-sky photometric calibration using bright stars

Photometric calibration to 5% accuracy is frequently needed at arbitrary celestial locations; however, existing all-sky astronomical catalogs do not reach this accuracy and time consuming photometric calibration procedures are required. I fit the Hipparcos B_T and V_T magnitudes along with the 2MASS J, H, and K magnitudes of Tycho-2 catalog-stars with stellar spectral templates. From the best fit spectral template derived for each star, I calculate the synthetic SDSS griz magnitudes and constructed an all-sky catalog of griz magnitudes for bright stars (V<12). Testing this method on SDSS photometric telescope observations, I find that the photometric accuracy for a single star is usually about 0.12, 0.12, 0.10 and 0.08 mag (1 sigma), for the g, r, i, and z-bands, respectively. However, by using ~10 such stars, the typical errors per calibrated field (systematic + statistical) can be reduced to about 0.04, 0.03, 0.02, and 0.02,mag, in the g, r, i, and z-bands, respectively. Therefore, in cases for which several calibration stars can be observed in the field of view of an instrument, accurate photometric calibration is possible.Comment: 3 pages, PASP, in pres