2001/02/15 by Masaru Watanabe, Naoki Yasuda, Nobunari Itoh +2 · 2 citations
Physics and Astronomy · #Astrophysics and Star Formation Studies #Galaxies: Formation, Evolution, Phenomena #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1086/321471
17pages, 23figures
arxiv created 2001/02/15 · openalex publication_date 2001/07/01 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/31
Infrared J and H surface photometry are carried out for nearby 12 galaxies whose distances have been accurately measured via Hubble Space Telescope Cepheid observations. Using the total, isophotal, and surface photometric aperture magnitudes, we calibrate the infrared luminosity-line-width relation (IRTF). It is found that IRTF changes its slope at log W ~ 2.45 in all the examined magnitude systems. The apparent scatter of IRTF is not significantly reduced when surface photometric magnitudes are used instead of the conventionally used synthetic aperture magnitude H -0.5 . It is also shown that the color ( I - H ) T of the nearby calibrator galaxies is redder by ~0.2 mag than the Coma Cluster of galaxies, but such a trend is not clearly visible for Ursa Major mostly because of poor statistics. The color offset of the Coma Cluster is analogous to that previously found in I T - H -0.5 . From the present calibration of H -band IRTF, we obtain the distance to the Coma Cluster to be m - M = 34.94 ± 0.13 mag, where no account is taken of the I - H color problem. Using the cosmic microwave background rest recession velocity of the Coma Cluster, we obtain H 0 = 73 ± 4 km s -1 Mpc -1 .