Other
Scientific paper
Apr 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994aj....107.1444s&link_type=abstract
The Astronomical Journal, vol. 107, no. 4, p. 1444-1452
Other
48
Light (Visible Radiation), Mathematical Models, Neutron Stars, Photometry, Red Shift, Solar Granulation, Spectroscopy, Supernovae, Astronomical Observatories, Atmospheric Correction, Bolometers, Charge Coupled Devices, Hubble Constant, Light Curve, Luminosity, Reflecting Telescopes
Scientific paper
We present photometry and spectroscopy of Supernova (SN) 1992am for five months following its discovery by the Calan Cerro-Tololo Inter-American Observatory (CTIO) SN search. These data show SN 1992am to be type II-P, displaying hydrogen in its spectrum and the typical shoulder in its light curve. The photometric data and the distance from our own analysis are used to construct the supernova's bolometric light curve. Using the bolometric light curve, we estimate SN 1992am ejected approximately 0.30 solar mass of Ni-56, an amount four times larger than that of other well studied SNe II. SN 1992am's; host galaxy lies at a redshift of cz = 14 600 km s-1, making it one of the most distant SNe II discovered, and an important application of the Expanding Photsphere Method. Since z = 0.05 is large enough for redshift-dependent effects to matter, we develop the technique to derive luminosity distances with the Expanding Photosphere Method at any redshift, and apply this method to SN 1992am. The derived distance, D = 180-25 +30 Mpc, is independent of all other rungs in the extragalactic distance ladder. The redshift of SN 1992am's host galaxy is sufficiently large that uncertainties due to perturbations in the smooth Hubble flow should be smaller than 10%. The Hubble ratio derived from the distance and redshift of this single object is H0 = 81-15 +17 km s-1 Mpc-1. In the future, with more of these distant objects, we hope to establish an independent and statistically robust estimate of H0 based solely on type II supernovae.
Aviles Roberto
Bolte Michael
Challis Peter
Eastman Ronald G.
Filippenko Alexei V.
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