SMHASH: Anatomy of the Orphan Stream using RR Lyrae stars

David Hendel, Victoria Scowcroft, Kathryn V. Johnston, Mark A. Fardal, Roeland P. van der Marel, Sangmo T. Sohn, Adrian M. Price-Whelan, Rachael L. Beaton, Gurtina Besla, Giuseppe Bono, Maria Rosa L. Cioni, Giselle Clementini, Judith G. Cohen, Michele Fabrizio, Wendy L. Freedman, Alessia Garofalo, Carl J. Grillmair, Nitya Kallivayalil, Juna A. Kollmeier, David R. LawBarry F. Madore, Steven R. Majewski, Massimo Marengo, Andrew J. Monson, Jillian R. Neeley, David L. Nidever, Grzegorz Pietrzyński, Mark Seibert, Branimir Sesar, Horace A. Smith, Igor Soszyński, Andrzej Udalski

Research output: Contribution to journalArticle

7 Scopus citations

Abstract

Stellar tidal streams provide an opportunity to study the motion and structure of the disrupting galaxy as well as the gravitational potential of its host. Streams around the Milky Way are especially promising as phase space positions of individual stars will be measured by ongoing or upcoming surveys. Nevertheless, it remains a challenge to accurately assess distances to stars farther than 10 kpc from the Sun, where we have the poorest knowledge of the Galaxy's mass distribution. To address this, we present observations of 32 candidate RR Lyrae stars in the Orphan tidal stream taken as part of the Spitzer Merger History and Shape of the Galactic Halo (SMHASH) program. The extremely tight correlation between the periods, luminosities, and metallicities of RR Lyrae variable stars in the Spitzer IRAC 3.6 μm band allows the determination of precise distances to individual stars; the median statistical relative distance uncertainty to each RR Lyrae star is 2.5 per cent. By fitting orbits in an example potential, we obtain an upper limit on the mass of the Milky Way interior to 60 kpc of 5.6 -1.1 + 1.2 × 1011 M, bringing estimates based on the Orphan Stream in line with those using other tracers. The SMHASH data also resolve the stream in line-of-sight depth, allowing a new perspective on the internal structure of the disrupted dwarf galaxy. Comparing with N-body models, we find that the progenitor had an initial dark halo mass of approximately 3.2 × 109M, placing the Orphan Stream's progenitor amongst the classical dwarf spheroidals.

Original languageEnglish (US)
Pages (from-to)570-587
Number of pages18
JournalMonthly Notices of the Royal Astronomical Society
Volume479
Issue number1
DOIs
StatePublished - Sep 1 2018

Keywords

  • Galaxy: halo
  • Galaxy: kinematics and dynamics
  • Galaxy: structure
  • Stars: variables: RR Lyrae

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

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    Hendel, D., Scowcroft, V., Johnston, K. V., Fardal, M. A., van der Marel, R. P., Sohn, S. T., Price-Whelan, A. M., Beaton, R. L., Besla, G., Bono, G., Cioni, M. R. L., Clementini, G., Cohen, J. G., Fabrizio, M., Freedman, W. L., Garofalo, A., Grillmair, C. J., Kallivayalil, N., Kollmeier, J. A., ... Udalski, A. (2018). SMHASH: Anatomy of the Orphan Stream using RR Lyrae stars. Monthly Notices of the Royal Astronomical Society, 479(1), 570-587. https://doi.org/10.1093/MNRAS/STY1455