Journal Article

The Early Palomar Program (1950–1955) for the Discovery of Classical Novae in M81: Analysis of the Spatial Distribution, Magnitude Distribution, and Distance Suggestion

Sandage, Allan, Zurek, David R., Shara, Michael M.

1999

Overview

Data obtained in the 1950–1955 Palomar campaign for the discovery of classical novae in M81 are set out in detail. Positions and apparentBmagnitudes are listed for the 23 novae that were found. There is modest evidence that the spatial distribution of the novae does not track theBbrightness distribution of either the total light or the light beyond an isophotal radius that is 70 \\documentclass{aastex} \\usepackage{amsbsy} \\usepackage{amsfonts} \\usepackage{amssymb} \\usepackage{bm} \\usepackage{mathrsfs} \\usepackage{pifont} \\usepackage{stmaryrd} \\usepackage{textcomp} \\usepackage{portland,xspace} \\usepackage{amsmath,amsxtra} \\usepackage[OT2,OT1]{fontenc} \\newcommand\\cyr{ \\renewcommand\\rmdefault{wncyr} \\renewcommand\\sfdefault{wncyss} \\renewcommand\\encodingdefault{OT2} \\normalfont \\selectfont} \\DeclareTextFontCommand{\\textcyr}{\\cyr} \\pagestyle{empty} \\DeclareMathSizes{10}{9}{7}{6} \\begin{document} \\landscape $\\arcsec$\\end{document} from the center of M81. The nova distribution is more extended than the aforementioned light, with a significant fraction of the sample appearing in the outer disk/spiral arm region. We suggest that many (perhaps a majority) of the M81 novae that are observed at any given epoch (compared with, say, 1010years ago) are daughters of Population I interacting binaries. The conclusion that the present‐day novae are drawn from two population groups—one from low‐mass white dwarf secondaries of close binaries identified with the bulge/thick disk population, and the other from massive white dwarf secondaries identified with the outer thin disk/spiral arm population—is discussed. We conclude that the M81 data are consistent with the two population division as argued previously from (1) observational studies on other grounds of nearby galaxies, (2) Monte Carlo simulations of novae in M31 and in the Galaxy, and (3) population synthesis modeling of nova binaries. Two different methods of using M81 novae as distance indicators give a nova distance modulus for M81 as (m− \\documentclass{aastex} \\usepackage{amsbsy} \\usepackage{amsfonts} \\usepackage{amssymb} \\usepackage{bm} \\usepackage{mathrsfs} \\usepackage{pifont} \\usepackage{stmaryrd} \\usepackage{textcomp} \\usepackage{portland,xspace} \\usepackage{amsmath,amsxtra} \\usepackage[OT2,OT1]{fontenc} \\newcommand\\cyr{ \\renewcommand\\rmdefault{wncyr} \\renewcommand\\sfdefault{wncyss} \\renewcommand\\encodingdefault{OT2} \\normalfont \\selectfont} \\DeclareTextFontCommand{\\textcyr}{\\cyr} \\pagestyle{empty} \\DeclareMathSizes{10}{9}{7}{6} \\begin{document} \\landscape $M) _{0}=27.75$ \\end{document} , consistent with the Cepheid modulus that is the same value.

• Publisher: The University of Chicago Press
• Subject: Andromeda Galaxy / Apparent magnitude / Cepheids / Galactic stellar content / Galaxies / Light curves / Milky Way Galaxy / Novae / Population distributions / White dwarfs