1998/10/01 by Mario Mateo, Edward W. Olszewski, Heather Morrison +1 · 2 citations
Physics and Astronomy · #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Dwarf galaxy #Dwarf spheroidal galaxy #Galactic Center #Galaxies: Formation, Evolution, Phenomena #Galaxy #Interacting galaxy #Physics #Sagittarius #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1086/311720
12 pages, 1 table, 2 figures at this site The large Fig 1 (140 kb compressed, 10 MEGABYTES uncompressed) is available at http://wharfrat.as.arizona.edu/~edo/MATEO_figure1.ps.gz Accepted by Ap. J. Letters
arxiv created 1998/10/01 · openalex publication_date 1998/11/20 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We have obtained deep photometric data in 24 fields along the southeast extension of the major axis of the Sagittarius dwarf spheroidal (Sgr dSph) galaxy and in four fields along the northwest extension. Using star counts at the expected position of the Sgr upper main sequence within the resulting color-magnitude diagrams, we unambiguously detect Sgr stars in the southeast over the range 10°-34° from the galaxy's center. If Sgr is symmetric, this implies a true major-axis diameter of at least 68°, or nearly 30 kpc if all portions of Sgr are equally distant from the Sun. Star counts parallel to the galaxy's minor axis reveal that Sgr remains quite broad far from its center. This suggests that the outer portions of Sgr resemble a stream rather than an extension of the ellipsoidal inner regions of the galaxy. The inferred V -band surface brightness (SB) profile ranges from 27.3 to 30.5 mag arcsec -2 over this radial range and exhibits a change in slope ~20° from the center of Sgr. The scale length of the outer SB profile is 17 2, compared with 4 7 in the central region of Sgr. We speculate that this break in the SB profile represents a transition from the main body of Sgr to a more extended "Sgr stream." By integrating the SB profile, we estimate that the absolute visual magnitude of Sgr lies in the range -13.4 to -14.6, depending on the assumed structure of Sgr; an upper limit to the luminosity of Sgr is therefore L ~5.8 × 10 7 L ☉ . This result lowers the M / L V ratio inferred for Sgr down to ~10, which is consistent with values observed in the most luminous dSph companions of the Milky Way.