skip to main content
OSTI.GOV title logo U.S. Department of Energy
Office of Scientific and Technical Information

Title: New BVI {sub C} photometry of low-mass pleiades stars: Exploring the effects of rotation on broadband colors

Abstract

We present new BVI{sub C} photometry for 350 Pleiades proper motion members with 9 < V ≲ 17. Importantly, our new catalog includes a large number of K- and early M-type stars, roughly doubling the number of low-mass stars with well-calibrated Johnson/Cousins photometry in this benchmark cluster. We combine our new photometry with existing photometry from the literature to define a purely empirical isochrone at Pleiades age (≈100 Myr) extending from V = 9 to 17. We use the empirical isochrone to identify 48 new probable binaries and 14 likely nonmembers. The photometrically identified single stars are compared against their expected positions in the color-magnitude diagram (CMD). At 100 Myr, the mid K and early M stars are predicted to lie above the zero-age main sequence (ZAMS) having not yet reached the ZAMS. We find in the B – V versus V CMD that mid K and early M dwarfs are instead displaced below (or blueward of) the ZAMS. Using the stars' previously reported rotation periods, we find a highly statistically significant correlation between rotation period and CMD displacement, in the sense that the more rapidly rotating stars have the largest displacements in the B – V CMD.

Authors:
;  [1];  [2];  [3]
  1. Department of Physics and Astronomy, Vanderbilt University, VU Station B 1807, Nashville, TN 37235 (United States)
  2. U.S. Naval Observatory, 10391 West Naval Observatory Road, Flagstaff, AZ 86001-8521 (United States)
  3. Spitzer Science Center, California Institute of Technology, MC 220-6, Pasadena, CA 91125 (United States)
Publication Date:
OSTI Identifier:
22342283
Resource Type:
Journal Article
Resource Relation:
Journal Name: Astronomical Journal (New York, N.Y. Online); Journal Volume: 148; Journal Issue: 2; Other Information: Country of input: International Atomic Energy Agency (IAEA)
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; BENCHMARKS; CATALOGS; COLOR; COMPARATIVE EVALUATIONS; CORRELATIONS; MASS; PHOTOMETRY; PROPER MOTION; ROTATION; STARS; STARSPOTS

Citation Formats

Kamai, Brittany L., Stassun, Keivan G., Vrba, Frederick J., and Stauffer, John R. New BVI {sub C} photometry of low-mass pleiades stars: Exploring the effects of rotation on broadband colors. United States: N. p., 2014. Web. doi:10.1088/0004-6256/148/2/30.
Kamai, Brittany L., Stassun, Keivan G., Vrba, Frederick J., & Stauffer, John R. New BVI {sub C} photometry of low-mass pleiades stars: Exploring the effects of rotation on broadband colors. United States. doi:10.1088/0004-6256/148/2/30.
Kamai, Brittany L., Stassun, Keivan G., Vrba, Frederick J., and Stauffer, John R. Fri . "New BVI {sub C} photometry of low-mass pleiades stars: Exploring the effects of rotation on broadband colors". United States. doi:10.1088/0004-6256/148/2/30.
@article{osti_22342283,
title = {New BVI {sub C} photometry of low-mass pleiades stars: Exploring the effects of rotation on broadband colors},
author = {Kamai, Brittany L. and Stassun, Keivan G. and Vrba, Frederick J. and Stauffer, John R.},
abstractNote = {We present new BVI{sub C} photometry for 350 Pleiades proper motion members with 9 < V ≲ 17. Importantly, our new catalog includes a large number of K- and early M-type stars, roughly doubling the number of low-mass stars with well-calibrated Johnson/Cousins photometry in this benchmark cluster. We combine our new photometry with existing photometry from the literature to define a purely empirical isochrone at Pleiades age (≈100 Myr) extending from V = 9 to 17. We use the empirical isochrone to identify 48 new probable binaries and 14 likely nonmembers. The photometrically identified single stars are compared against their expected positions in the color-magnitude diagram (CMD). At 100 Myr, the mid K and early M stars are predicted to lie above the zero-age main sequence (ZAMS) having not yet reached the ZAMS. We find in the B – V versus V CMD that mid K and early M dwarfs are instead displaced below (or blueward of) the ZAMS. Using the stars' previously reported rotation periods, we find a highly statistically significant correlation between rotation period and CMD displacement, in the sense that the more rapidly rotating stars have the largest displacements in the B – V CMD.},
doi = {10.1088/0004-6256/148/2/30},
journal = {Astronomical Journal (New York, N.Y. Online)},
number = 2,
volume = 148,
place = {United States},
year = {Fri Aug 01 00:00:00 EDT 2014},
month = {Fri Aug 01 00:00:00 EDT 2014}
}