STELLAR ARCHAEOLOGY IN THE GALACTIC HALO WITH THE ULTRA-FAINT DWARFS. VI. URSA MAJOR II
We present a B, V color-magnitude diagram (CMD) of the Milky Way dwarf satellite Ursa Major II (UMa II), spanning the magnitude range from V ~ 15 to V ~ 23.5 mag and extending over an 18 x 18 arcmin super(2) area centered on the Galaxy. Our photometry goes down to about 2 mag below the Galaxy's...
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| Veröffentlicht in: | The Astrophysical journal 2012-06, Vol.752 (1), p.1-9 |
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| creator | DALL'ORA, M KINEMUCHI, Karen KUEHN, Charles A CATELAN, Márcio PRITZL, Barton J BEERS, Timothy C RIPEPI, Vincenzo RODGERS, Christopher T CLEMENTINI, Gisella DI FABRIZIO, Luca SMITH, Horace A MARCONI, Marcella MUSELLA, Ilaria GRECO, Claudia |
| description | We present a B, V color-magnitude diagram (CMD) of the Milky Way dwarf satellite Ursa Major II (UMa II), spanning the magnitude range from V ~ 15 to V ~ 23.5 mag and extending over an 18 x 18 arcmin super(2) area centered on the Galaxy. Our photometry goes down to about 2 mag below the Galaxy's main-sequence turnoff that we detected at V ~ 21.5 mag. We have discovered a bona fide RR Lyrae variable star in UMa II, which we use to estimate a conservative dereddened distance modulus for the galaxy of (m - M) sub(0) = 17.70 + or - 0.04 + or - 0.12mag, where the first error accounts for the uncertainties of the calibrated photometry, and the second reflects our lack of information on the metallicity of the star. The corresponding distance to UMa II is 34.7 super(+0.6) sub(-0.7)( super(+2.0) sub(-1.9)) kpc. Our photometry shows evidence of a spread in the Galaxy's subgiant branch, compatible with a spread in metal abundance in the range between Z = 0.0001 and Z = 0.001. Based on our estimate of the distance, a comparison of the fiducial lines of the Galactic globular clusters M68 and M5 ([Fe/H] = -2.27 + or - 0.04 dex and -1.33 + or - 0.02 dex, respectively), with the position on the CMD of spectroscopically confirmed Galaxy members, may suggest the existence of stellar populations of different metal abundance/age in the central region of UMa II. |
| doi_str_mv | 10.1088/0004-637X/752/1/42 |
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VI. URSA MAJOR II</title><source>IOP Publishing Free Content</source><source>Elektronische Zeitschriftenbibliothek - Frei zugängliche E-Journals</source><source>Alma/SFX Local Collection</source><creator>DALL'ORA, M ; KINEMUCHI, Karen ; KUEHN, Charles A ; CATELAN, Márcio ; PRITZL, Barton J ; BEERS, Timothy C ; RIPEPI, Vincenzo ; RODGERS, Christopher T ; CLEMENTINI, Gisella ; DI FABRIZIO, Luca ; SMITH, Horace A ; MARCONI, Marcella ; MUSELLA, Ilaria ; GRECO, Claudia</creator><creatorcontrib>DALL'ORA, M ; KINEMUCHI, Karen ; KUEHN, Charles A ; CATELAN, Márcio ; PRITZL, Barton J ; BEERS, Timothy C ; RIPEPI, Vincenzo ; RODGERS, Christopher T ; CLEMENTINI, Gisella ; DI FABRIZIO, Luca ; SMITH, Horace A ; MARCONI, Marcella ; MUSELLA, Ilaria ; GRECO, Claudia</creatorcontrib><description>We present a B, V color-magnitude diagram (CMD) of the Milky Way dwarf satellite Ursa Major II (UMa II), spanning the magnitude range from V ~ 15 to V ~ 23.5 mag and extending over an 18 x 18 arcmin super(2) area centered on the Galaxy. Our photometry goes down to about 2 mag below the Galaxy's main-sequence turnoff that we detected at V ~ 21.5 mag. We have discovered a bona fide RR Lyrae variable star in UMa II, which we use to estimate a conservative dereddened distance modulus for the galaxy of (m - M) sub(0) = 17.70 + or - 0.04 + or - 0.12mag, where the first error accounts for the uncertainties of the calibrated photometry, and the second reflects our lack of information on the metallicity of the star. The corresponding distance to UMa II is 34.7 super(+0.6) sub(-0.7)( super(+2.0) sub(-1.9)) kpc. Our photometry shows evidence of a spread in the Galaxy's subgiant branch, compatible with a spread in metal abundance in the range between Z = 0.0001 and Z = 0.001. Based on our estimate of the distance, a comparison of the fiducial lines of the Galactic globular clusters M68 and M5 ([Fe/H] = -2.27 + or - 0.04 dex and -1.33 + or - 0.02 dex, respectively), with the position on the CMD of spectroscopically confirmed Galaxy members, may suggest the existence of stellar populations of different metal abundance/age in the central region of UMa II.</description><identifier>ISSN: 0004-637X</identifier><identifier>EISSN: 1538-4357</identifier><identifier>DOI: 10.1088/0004-637X/752/1/42</identifier><identifier>CODEN: ASJOAB</identifier><language>eng</language><publisher>Bristol: IOP</publisher><subject>Abundance ; ASTRONOMY ; ASTROPHYSICS ; ASTROPHYSICS, COSMOLOGY AND ASTRONOMY ; COLOR ; COMPARATIVE EVALUATIONS ; DIAGRAMS ; DISTANCE ; Earth, ocean, space ; ELEMENT ABUNDANCE ; Estimates ; Exact sciences and technology ; Galactic halos ; HYDROGEN ; IRON ; Metallicity ; MILKY WAY ; Milky Way Galaxy ; PHOTOMETRY ; Spreads ; STAR CLUSTERS ; VARIABLE STARS</subject><ispartof>The Astrophysical journal, 2012-06, Vol.752 (1), p.1-9</ispartof><rights>2015 INIST-CNRS</rights><lds50>peer_reviewed</lds50><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed><citedby>FETCH-LOGICAL-c345t-acc6287f778fec669cd22be8e8b825ece68d26f1247ca9956328ee5ef90794593</citedby></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>230,314,776,780,881,27901,27902</link.rule.ids><backlink>$$Uhttp://pascal-francis.inist.fr/vibad/index.php?action=getRecordDetail&idt=26304951$$DView record in Pascal Francis$$Hfree_for_read</backlink><backlink>$$Uhttps://www.osti.gov/biblio/22037077$$D View this record in Osti.gov$$Hfree_for_read</backlink></links><search><creatorcontrib>DALL'ORA, M</creatorcontrib><creatorcontrib>KINEMUCHI, Karen</creatorcontrib><creatorcontrib>KUEHN, Charles A</creatorcontrib><creatorcontrib>CATELAN, Márcio</creatorcontrib><creatorcontrib>PRITZL, Barton J</creatorcontrib><creatorcontrib>BEERS, Timothy C</creatorcontrib><creatorcontrib>RIPEPI, Vincenzo</creatorcontrib><creatorcontrib>RODGERS, Christopher T</creatorcontrib><creatorcontrib>CLEMENTINI, Gisella</creatorcontrib><creatorcontrib>DI FABRIZIO, Luca</creatorcontrib><creatorcontrib>SMITH, Horace A</creatorcontrib><creatorcontrib>MARCONI, Marcella</creatorcontrib><creatorcontrib>MUSELLA, Ilaria</creatorcontrib><creatorcontrib>GRECO, Claudia</creatorcontrib><title>STELLAR ARCHAEOLOGY IN THE GALACTIC HALO WITH THE ULTRA-FAINT DWARFS. VI. URSA MAJOR II</title><title>The Astrophysical journal</title><description>We present a B, V color-magnitude diagram (CMD) of the Milky Way dwarf satellite Ursa Major II (UMa II), spanning the magnitude range from V ~ 15 to V ~ 23.5 mag and extending over an 18 x 18 arcmin super(2) area centered on the Galaxy. Our photometry goes down to about 2 mag below the Galaxy's main-sequence turnoff that we detected at V ~ 21.5 mag. We have discovered a bona fide RR Lyrae variable star in UMa II, which we use to estimate a conservative dereddened distance modulus for the galaxy of (m - M) sub(0) = 17.70 + or - 0.04 + or - 0.12mag, where the first error accounts for the uncertainties of the calibrated photometry, and the second reflects our lack of information on the metallicity of the star. The corresponding distance to UMa II is 34.7 super(+0.6) sub(-0.7)( super(+2.0) sub(-1.9)) kpc. Our photometry shows evidence of a spread in the Galaxy's subgiant branch, compatible with a spread in metal abundance in the range between Z = 0.0001 and Z = 0.001. Based on our estimate of the distance, a comparison of the fiducial lines of the Galactic globular clusters M68 and M5 ([Fe/H] = -2.27 + or - 0.04 dex and -1.33 + or - 0.02 dex, respectively), with the position on the CMD of spectroscopically confirmed Galaxy members, may suggest the existence of stellar populations of different metal abundance/age in the central region of UMa II.</description><subject>Abundance</subject><subject>ASTRONOMY</subject><subject>ASTROPHYSICS</subject><subject>ASTROPHYSICS, COSMOLOGY AND ASTRONOMY</subject><subject>COLOR</subject><subject>COMPARATIVE EVALUATIONS</subject><subject>DIAGRAMS</subject><subject>DISTANCE</subject><subject>Earth, ocean, space</subject><subject>ELEMENT ABUNDANCE</subject><subject>Estimates</subject><subject>Exact sciences and technology</subject><subject>Galactic halos</subject><subject>HYDROGEN</subject><subject>IRON</subject><subject>Metallicity</subject><subject>MILKY WAY</subject><subject>Milky Way Galaxy</subject><subject>PHOTOMETRY</subject><subject>Spreads</subject><subject>STAR CLUSTERS</subject><subject>VARIABLE STARS</subject><issn>0004-637X</issn><issn>1538-4357</issn><fulltext>true</fulltext><rsrctype>article</rsrctype><creationdate>2012</creationdate><recordtype>article</recordtype><recordid>eNqNkU1Lw0AQhhdRsFb_gKcFEbyk3e-P4xJbE4kW0tTqaYnrBiNto9n04L83tcWzp2GG531neAeAS4xGGCk1RgixSFD5PJacjPGYkSMwwJyqiFEuj8HgDzgFZyF87Fqi9QAs58Uky0wOTR4nZjLLZncvMH2ERTKBdyYzcZHGMDHZDC7TIvkdL7IiN9HUpI8FvF2afDofwad0BBf53MAHcz_LYZqeg5OqXAV_cahDsJhOijiJ-gVpbLLIUca7qHROECUrKVXlnRDavRHy6pVXr4pw77xQb0RUmDDpSq25oER5z32lkdSMazoEV3vfJnS1Da7uvHt3zWbjXWcJQVQiKXvqZk99ts3X1ofOruvg_GpVbnyzDRZLpPsTGMP_QTFTSDDUo2SPurYJofWV_Wzrddl-W4zs7i12F7PdpW77t1hsGelF1wf_MrhyVbXlxtXhT0kERUxzTH8AgneC1g</recordid><startdate>20120610</startdate><enddate>20120610</enddate><creator>DALL'ORA, M</creator><creator>KINEMUCHI, Karen</creator><creator>KUEHN, Charles A</creator><creator>CATELAN, Márcio</creator><creator>PRITZL, Barton J</creator><creator>BEERS, Timothy C</creator><creator>RIPEPI, Vincenzo</creator><creator>RODGERS, Christopher T</creator><creator>CLEMENTINI, Gisella</creator><creator>DI FABRIZIO, Luca</creator><creator>SMITH, Horace A</creator><creator>MARCONI, Marcella</creator><creator>MUSELLA, Ilaria</creator><creator>GRECO, Claudia</creator><general>IOP</general><scope>IQODW</scope><scope>AAYXX</scope><scope>CITATION</scope><scope>7TG</scope><scope>KL.</scope><scope>8FD</scope><scope>H8D</scope><scope>L7M</scope><scope>OTOTI</scope></search><sort><creationdate>20120610</creationdate><title>STELLAR ARCHAEOLOGY IN THE GALACTIC HALO WITH THE ULTRA-FAINT DWARFS. 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VI. URSA MAJOR II</atitle><jtitle>The Astrophysical journal</jtitle><date>2012-06-10</date><risdate>2012</risdate><volume>752</volume><issue>1</issue><spage>1</spage><epage>9</epage><pages>1-9</pages><issn>0004-637X</issn><eissn>1538-4357</eissn><coden>ASJOAB</coden><abstract>We present a B, V color-magnitude diagram (CMD) of the Milky Way dwarf satellite Ursa Major II (UMa II), spanning the magnitude range from V ~ 15 to V ~ 23.5 mag and extending over an 18 x 18 arcmin super(2) area centered on the Galaxy. Our photometry goes down to about 2 mag below the Galaxy's main-sequence turnoff that we detected at V ~ 21.5 mag. We have discovered a bona fide RR Lyrae variable star in UMa II, which we use to estimate a conservative dereddened distance modulus for the galaxy of (m - M) sub(0) = 17.70 + or - 0.04 + or - 0.12mag, where the first error accounts for the uncertainties of the calibrated photometry, and the second reflects our lack of information on the metallicity of the star. The corresponding distance to UMa II is 34.7 super(+0.6) sub(-0.7)( super(+2.0) sub(-1.9)) kpc. Our photometry shows evidence of a spread in the Galaxy's subgiant branch, compatible with a spread in metal abundance in the range between Z = 0.0001 and Z = 0.001. Based on our estimate of the distance, a comparison of the fiducial lines of the Galactic globular clusters M68 and M5 ([Fe/H] = -2.27 + or - 0.04 dex and -1.33 + or - 0.02 dex, respectively), with the position on the CMD of spectroscopically confirmed Galaxy members, may suggest the existence of stellar populations of different metal abundance/age in the central region of UMa II.</abstract><cop>Bristol</cop><pub>IOP</pub><doi>10.1088/0004-637X/752/1/42</doi><tpages>9</tpages><oa>free_for_read</oa></addata></record> |
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| subjects | Abundance ASTRONOMY ASTROPHYSICS ASTROPHYSICS, COSMOLOGY AND ASTRONOMY COLOR COMPARATIVE EVALUATIONS DIAGRAMS DISTANCE Earth, ocean, space ELEMENT ABUNDANCE Estimates Exact sciences and technology Galactic halos HYDROGEN IRON Metallicity MILKY WAY Milky Way Galaxy PHOTOMETRY Spreads STAR CLUSTERS VARIABLE STARS |
| title | STELLAR ARCHAEOLOGY IN THE GALACTIC HALO WITH THE ULTRA-FAINT DWARFS. VI. URSA MAJOR II |
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