Determining the location of the tip of the red giant branch in old stellar populations: M33, Andromeda I and II
Identifieur interne : 001692 ( Istex/Curation ); précédent : 001691; suivant : 001693Determining the location of the tip of the red giant branch in old stellar populations: M33, Andromeda I and II
Auteurs : A. W. Mcconnachie [Royaume-Uni] ; M. J. Irwin ; A. M. N. Ferguson [Allemagne] ; R. A. Ibata [France] ; G. F. Lewis [Australie] ; N. TanvirSource :
- Monthly Notices of the Royal Astronomical Society [ 0035-8711 ] ; 2004-05.
English descriptors
- KwdEn :
- Absolute magnitude, Adaptive, Adaptive slope, Algorithm, Andromeda, Annulus, Apparent magnitude, Background contaminants, Binned luminosity function, Brighter magnitudes, Cepheid distances, Constant error term, Contour plot, Core helium ignition, Costa, Distance indicator, Distance modulus, Dwarf galaxies andromeda, Edge detection algorithm, Eld, Elliptical annulus, Excellent agreement, Foreground, Foreground stars, Freedman, Galaxy, Giant branch, Girardi, Girardi salaris, Good agreement, Group galaxies, Heuristic, Heuristic method, Interstellar reddening, Intrinsic shape, Irwin, Larger numbers, Local foreground correction, Lower panel, Luminosity, Luminosity function, Luminosity functions, Madore, Madore freedman, Maximum likelihood method, Mcconnachie, Metallicity, Mnras, Negligible effect, Neighbouring, Neighbouring bins, Neighbouring star counts, Noise effects, Photometric, Photometric conditions, Photometric error, Poisson, Poisson noise, Previous estimates, Previous methods, Real data, Reasonable agreement, Reasonable approximation, Right panel, Simple slope function, Sobel edge detection algorithm, Sobel kernel, Solid line, Spiral galaxy, Standard candle, Star counts, Statistical correction, Stellar, Stellar evolution, Stellar population, Stellar systems, Theoretical predictions, Trgb, Trgb distance determinations, Trgb distance determinations figure, Trgb edge, Trgb location, Trgb measurement, Tting procedure, Twentieth magnitude, Upper panel, Wide field camera.
- Teeft :
- Absolute magnitude, Adaptive, Adaptive slope, Algorithm, Andromeda, Annulus, Apparent magnitude, Background contaminants, Binned luminosity function, Brighter magnitudes, Cepheid distances, Constant error term, Contour plot, Core helium ignition, Costa, Distance indicator, Distance modulus, Dwarf galaxies andromeda, Edge detection algorithm, Eld, Elliptical annulus, Excellent agreement, Foreground, Foreground stars, Freedman, Galaxy, Giant branch, Girardi, Girardi salaris, Good agreement, Group galaxies, Heuristic, Heuristic method, Interstellar reddening, Intrinsic shape, Irwin, Larger numbers, Local foreground correction, Lower panel, Luminosity, Luminosity function, Luminosity functions, Madore, Madore freedman, Maximum likelihood method, Mcconnachie, Metallicity, Mnras, Negligible effect, Neighbouring, Neighbouring bins, Neighbouring star counts, Noise effects, Photometric, Photometric conditions, Photometric error, Poisson, Poisson noise, Previous estimates, Previous methods, Real data, Reasonable agreement, Reasonable approximation, Right panel, Simple slope function, Sobel edge detection algorithm, Sobel kernel, Solid line, Spiral galaxy, Standard candle, Star counts, Statistical correction, Stellar, Stellar evolution, Stellar population, Stellar systems, Theoretical predictions, Trgb, Trgb distance determinations, Trgb distance determinations figure, Trgb edge, Trgb location, Trgb measurement, Tting procedure, Twentieth magnitude, Upper panel, Wide field camera.
Abstract
The absolute bolometric luminosity of the point of core helium ignition in old, metal‐poor, red giant stars is of roughly constant magnitude, varying only very slightly with mass or metallicity It can thus be used as a standard candle. Here, we review the main difficulties in measuring this location in any real data set and we develop an empirical approach to optimize it for tip of the red giant branch (TRGB) analysis. We go on to present a new algorithm for the identification of the TRGB in nearby metal‐poor stellar systems. Our method uses a least‐squares fit of a data adaptive slope to the luminosity function in 1‐mag windows. This finds the region of the luminosity function that shows the most significant decline in star counts as we go to brighter magnitudes; the base of this decline is attributed as the location of the tip. This technique then allows for the determination of realistic uncertainties which reflect the quality of the luminosity function used, but which are typically ∼0.02 mag rms +∼0.03 mag systematic, a significant improvement upon previous methods that have used the tip as a standard candle. Finally, we apply our technique to the Local Group spiral galaxy M33 and the dwarf galaxies Andromeda I and II, and derive distance modulii of 24.50 ± 0.06 mag (794 ± 23 kpc), 24.33 ± 0.07 mag (735 ± 23 kpc) and 24.05 ± 0.06 mag (645 ± 19 kpc) respectively. The result for M33 is in excellent agreement with the Cepheid distances to this galaxy, and makes the possibility of a significant amount of reddening in this object unlikely.
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DOI: 10.1111/j.1365-2966.2004.07637.x
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M. J. Irwin<affiliation><mods:affiliation>Institute of Astronomy, Madingley Road, Cambridge CB3 0HA</mods:affiliation><wicri:noCountry code="subField">0HA</wicri:noCountry></affiliation><affiliation><mods:affiliation>Physics, Astronomy and Mathematics Department, University of Hertfordshire, Hatfield AL10 9AB</mods:affiliation><wicri:noCountry code="subField">9AB</wicri:noCountry></affiliation>Le document en format XML
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Telephone (0131) 226 7232 Fax (0131) 226 3803 </pubPlace><date type="published" when="2004-05">2004-05</date></imprint><idno type="ISSN">0035-8711</idno></series></biblStruct></sourceDesc><seriesStmt><idno type="ISSN">0035-8711</idno></seriesStmt></fileDesc><profileDesc><textClass><keywords scheme="KwdEn" xml:lang="en"><term>Absolute magnitude</term><term>Adaptive</term><term>Adaptive slope</term><term>Algorithm</term><term>Andromeda</term><term>Annulus</term><term>Apparent magnitude</term><term>Background contaminants</term><term>Binned luminosity function</term><term>Brighter magnitudes</term><term>Cepheid distances</term><term>Constant error term</term><term>Contour plot</term><term>Core helium ignition</term><term>Costa</term><term>Distance indicator</term><term>Distance modulus</term><term>Dwarf galaxies andromeda</term><term>Edge detection algorithm</term><term>Eld</term><term>Elliptical annulus</term><term>Excellent agreement</term><term>Foreground</term><term>Foreground stars</term><term>Freedman</term><term>Galaxy</term><term>Giant branch</term><term>Girardi</term><term>Girardi salaris</term><term>Good agreement</term><term>Group galaxies</term><term>Heuristic</term><term>Heuristic method</term><term>Interstellar reddening</term><term>Intrinsic shape</term><term>Irwin</term><term>Larger numbers</term><term>Local foreground correction</term><term>Lower panel</term><term>Luminosity</term><term>Luminosity function</term><term>Luminosity functions</term><term>Madore</term><term>Madore freedman</term><term>Maximum likelihood method</term><term>Mcconnachie</term><term>Metallicity</term><term>Mnras</term><term>Negligible effect</term><term>Neighbouring</term><term>Neighbouring bins</term><term>Neighbouring star counts</term><term>Noise effects</term><term>Photometric</term><term>Photometric conditions</term><term>Photometric error</term><term>Poisson</term><term>Poisson noise</term><term>Previous estimates</term><term>Previous methods</term><term>Real data</term><term>Reasonable agreement</term><term>Reasonable approximation</term><term>Right panel</term><term>Simple slope function</term><term>Sobel edge detection algorithm</term><term>Sobel kernel</term><term>Solid line</term><term>Spiral galaxy</term><term>Standard candle</term><term>Star counts</term><term>Statistical correction</term><term>Stellar</term><term>Stellar evolution</term><term>Stellar population</term><term>Stellar systems</term><term>Theoretical predictions</term><term>Trgb</term><term>Trgb distance determinations</term><term>Trgb distance determinations figure</term><term>Trgb edge</term><term>Trgb location</term><term>Trgb measurement</term><term>Tting procedure</term><term>Twentieth magnitude</term><term>Upper panel</term><term>Wide field camera</term></keywords><keywords scheme="Teeft" xml:lang="en"><term>Absolute magnitude</term><term>Adaptive</term><term>Adaptive slope</term><term>Algorithm</term><term>Andromeda</term><term>Annulus</term><term>Apparent magnitude</term><term>Background contaminants</term><term>Binned luminosity function</term><term>Brighter magnitudes</term><term>Cepheid distances</term><term>Constant error term</term><term>Contour plot</term><term>Core helium ignition</term><term>Costa</term><term>Distance indicator</term><term>Distance modulus</term><term>Dwarf galaxies andromeda</term><term>Edge detection algorithm</term><term>Eld</term><term>Elliptical annulus</term><term>Excellent agreement</term><term>Foreground</term><term>Foreground stars</term><term>Freedman</term><term>Galaxy</term><term>Giant branch</term><term>Girardi</term><term>Girardi salaris</term><term>Good agreement</term><term>Group galaxies</term><term>Heuristic</term><term>Heuristic method</term><term>Interstellar reddening</term><term>Intrinsic shape</term><term>Irwin</term><term>Larger numbers</term><term>Local foreground correction</term><term>Lower panel</term><term>Luminosity</term><term>Luminosity function</term><term>Luminosity functions</term><term>Madore</term><term>Madore freedman</term><term>Maximum likelihood method</term><term>Mcconnachie</term><term>Metallicity</term><term>Mnras</term><term>Negligible effect</term><term>Neighbouring</term><term>Neighbouring bins</term><term>Neighbouring star counts</term><term>Noise effects</term><term>Photometric</term><term>Photometric conditions</term><term>Photometric error</term><term>Poisson</term><term>Poisson noise</term><term>Previous estimates</term><term>Previous methods</term><term>Real data</term><term>Reasonable agreement</term><term>Reasonable approximation</term><term>Right panel</term><term>Simple slope function</term><term>Sobel edge detection algorithm</term><term>Sobel kernel</term><term>Solid line</term><term>Spiral galaxy</term><term>Standard candle</term><term>Star counts</term><term>Statistical correction</term><term>Stellar</term><term>Stellar evolution</term><term>Stellar population</term><term>Stellar systems</term><term>Theoretical predictions</term><term>Trgb</term><term>Trgb distance determinations</term><term>Trgb distance determinations figure</term><term>Trgb edge</term><term>Trgb location</term><term>Trgb measurement</term><term>Tting procedure</term><term>Twentieth magnitude</term><term>Upper panel</term><term>Wide field camera</term></keywords></textClass></profileDesc></teiHeader><front><div type="abstract" xml:lang="en">The absolute bolometric luminosity of the point of core helium ignition in old, metal‐poor, red giant stars is of roughly constant magnitude, varying only very slightly with mass or metallicity It can thus be used as a standard candle. Here, we review the main difficulties in measuring this location in any real data set and we develop an empirical approach to optimize it for tip of the red giant branch (TRGB) analysis. We go on to present a new algorithm for the identification of the TRGB in nearby metal‐poor stellar systems. Our method uses a least‐squares fit of a data adaptive slope to the luminosity function in 1‐mag windows. This finds the region of the luminosity function that shows the most significant decline in star counts as we go to brighter magnitudes; the base of this decline is attributed as the location of the tip. This technique then allows for the determination of realistic uncertainties which reflect the quality of the luminosity function used, but which are typically ∼0.02 mag rms +∼0.03 mag systematic, a significant improvement upon previous methods that have used the tip as a standard candle. Finally, we apply our technique to the Local Group spiral galaxy M33 and the dwarf galaxies Andromeda I and II, and derive distance modulii of 24.50 ± 0.06 mag (794 ± 23 kpc), 24.33 ± 0.07 mag (735 ± 23 kpc) and 24.05 ± 0.06 mag (645 ± 19 kpc) respectively. The result for M33 is in excellent agreement with the Cepheid distances to this galaxy, and makes the possibility of a significant amount of reddening in this object unlikely.</div></front></TEI></record>Pour manipuler ce document sous Unix (Dilib)
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