29 1 Vol.29, No. 1 2011 1 PROGRESS IN ASTRONOMY Jan., 2011 1000-8349(2011)01-0031-15 1,2 1,3 1 1 ( 1. 200030 2. 100049 3. 200234 ) (red clump giant) (Hipparcos) P145.2 A 1 [1] 1970 Cannon [2] Cannon [2] 2010-4-14 2010-5-24 (10773021 10833005) (10821302) 973 (2007CB815402/403)
32 29 0.5 2.3 M (M cr 0.45 M ) 10 8 K ( ) 0.5 M [3] [2] ( 1) II (horizontal branch) [4] ( 2) Hipparcos [6] ( 3) Cannon [2] 1970 2 Hipparcos [6] Hipparcos I K 3 ( ) V [7 9] [8, 10, 11, 13] I K [13, 15, 18, 19] I K 2.1 1998 Paczyński Stanek [10] 10% Hipparcos ( 4) 600 I ( 0.185 ± 0.016) mag ( 0.279 ± 0.088) mag 0.2 mag 0.8 < (V I) 0 < 1.4
1 33 1 NGC 7789 NGC 2158 5 2MASS [5] 4 N RC n(i 0 ) = a + b(i 0 I 0,m ) + exp [ (I ] 0 I 0,m ) 2, (1) σ RC 2π 2σ 2 RC (1) a b n(i 0 ) N RC I 0 I 0,m σ RC 1998 Stanek Garnavich [16] Paczyński Stanek [10] n(i 0 ) = a + b(i 0 I 0,m ) + c(i 0 I 0,m ) 2 N RC + exp [ (I ] 0 I 0,m ) 2 σ RC 2π 2σ 2 RC, (2) (2) (1) I ( 0.23 ± 0.03) mag 0.2 mag
34 29 2 47 Tuc 3 2MASS [5] 3 B V M V 15 091 σ π /π < 10% σ B V < 0.025 mag 100 pc
1 35 4 10% I (1) [10] 1998 Kaluzny [17] Stanek Garnavich [16] 47 Tuc I Stanek Garnavich [16] ( 0.23 ± 0.03) mag 47 Tuc 0.2 0.25 mag Kaluzny [17] 47 Tuc Hipparcos [Fe/H] 0.7 dex I 0.48 mag 1999 Sarajedini [8] 10 0.4 [Fe/H] 0.2 2 9 Ga V I V M V = m V A V (m M) 0, (3) M V m V A V (m M) 0 V (3) I V I Sarajedini [8] 10 V I
36 29 M V = 0.84 mag 0.24 mag M I = 0.19 mag 0.16 mag Sarajedini [8] M V M I 2000 Udalski [11] 284 Hipparcos (σ π /π < 10%) I M I = (0.13±0.07)([Fe/H]+0.25) + ( 0.26 ± 0.02) 0.6 [Fe/H] 0.2 dex Zhao [12] 39 Hipparcos 39 Udalski [11] M I = (0.12 ± 0.11)([Fe/H]+0.25) + ( 0.18 ± 0.04) I 2008 Groenewegen [13] Hipparcos Hipparcos I ( 0.22 ± 0.03) mag 0.20 mag I (V I) 0 2.2 K 2000 Alves [15] K Alves [15] 238 Hipparcos (σ π /π < 10% 5%) ( 0.1 dex) Alves K ( 1.61 ± 0.03) mag (0.22 ± 0.03) mag K M K = (0.57 ± 0.36)[Fe/H] (1.64 ± 0.07) 2002 Grocholski [18] 14 K K (3) Grocholski [18] 14 M K = 1.62 ± 0.06 mag 0.21 mag 2 Ga K 2 Ga K I 2007 Van Helshoecht [19] Grocholski [18] 14 26 2 Grocholski [18] K Van Helshoecht [19] M K (RC)= 1.57 ± 0.05 mag 0.25 mag 0.5 0.4 10 8.5 10 9.9 a K 2008 Groenewegen [13] Hipparcos Hipparcos K (2MASS ) ( 1.54 ± 0.04) mag 0.22 mag K (V K) 0
1 37 3 3.1 R ( ) R Oort R A R H 0 R [20] [20] 1998 Paczyński Stanek [10] Hipparcos Baade Paczyński Stanek [10] ( 10%) Hipparcos I (OGLE) Baade I ( 5) ( (4)) (m M) GC = (14.62 ± 0.1) mag R = (8.4 ± 0.4) kpc Hipparcos 600 Baade 10 000 1% Paczyński Stanek [10] (4) (m M) 0 = m λ M λ A λ + M λ (4) (m M) 0 m λ M λ A λ M λ 1998 Stanek Garnavich [16] Paczyński Stanek [10] Hipparcos (14.57 ± 0.04 ± 0.04) mag ( + ) R = (8.2 ± 0.15 ± 0.15) kpc 2000 Alves [15] 238 Hipparcos K ( 1.61± 0.03) mag Tiede [21] Baade K (14.58 ± 0.11) mag R = (8.24 ± 0.42) kpc 238 Baade Alves [15] Baade 2006 Nishiyama [22] IRSF SIRIUS
38 29 5 Baade Hipparcos 5 5 (1) ( (1) [10] l 1.0 0.7 b 1.0 J H Ks Alves [15] Hipparcos K (14.38 ± 0.03 ± 0.10) mag ( + ) R = (7.52 ± 0.10 ± 0.35) kpc Nishiyama [22] Hipparcos ( 0.07 mag) Nishiyama [22] Hipparcos Nishiyama [22] Eisenhauer [23] R = (7.62 ± 0.32) kpc Eisenhauer [23] 5% 1 3.2
1 39 1 /mag R /kpc 1 14.62 ± 0.1 8.4 ± 0.4 1998 [10] I 2 14.57 ± 0.04 ± 0.04 8.2 ± 0.15 ± 0.15 1998 [16] I 3 14.58 ± 0.11 8.24 ± 0.42 2000 [15] K 4 14.38 ± 0.03 ± 0.10 7.52 ± 0.10 ± 0.35 2006 [22] K 1964 de Vaucouleurs [24] HI 2009 Zhao [25] 1994 Stanek [26] OGLE ( ) 13 5 10 5 13 9 Baade Baade 4 l ±5 (0.37 ± 0.03) mag (1.185 ± 0.015) Stanek [26] 45 1997 Stanek [27] OGLE 12 7 10 5 20 30 3.5 : 1.5 : 1 2005 Nishiyama [28] IRSF SIRIUS 10.5 l 10.5 b = 1 l = 10 13.4 mag l = 10 12.2 mag Nishiyama [28] 4 l 4 0.1 mag 2005 Babusiaux Gilmore [29] 22 ± 5.5 2.5 kpc Babusiaux Gilmore [29] 2
40 29 2007 Rattenbury [30] OGLE-II 44-24 27 10 : 3.5 : 2.6 Cabrera-Lavers [31] 2MASS 5 kpc b < 2 43.0 ± 1.8 100 pc b 7.5 12.6 ± 3.2 5 2008 Cabrera-Lavers [32] UKIDSS-GPS (United Kingdom Infrared Deep Sky Survey- Galactic Plane Survey) l = 10 23.60 ± 2.19 l 10 l = 28 42.44 ± 2.14 3.3 (LMC) LMC [33] LMC LMC [33] LMC 1998 Udalski [34] OGLE-II Paczyński Stanek [10] LMC 4 4 LMC LMC (18.08 ± 0.03 ± 0.12) mag ( + ) 20 000 RR SN1987A (light echo) (18.50 ± 0.15) mag [35] 0.4 mag 15% (SMC) 0.4 mag Udalski [34] (population effects) 0.4 mag Udalski [34] Stanek [36] Udalski [34] Stanek [36] Udalski [34] Stanek Garnavich Hipparcos [16] LMC (18.065 ± 0.031 ± 0.09) mag ( + ) R LMC = (41.02 ± 0.59 ± 1.74) kpc Stanek [36] Udalski [34] LMC 0.4 mag Stanek [36] LMC
1 41 Hipparcos 1998 Cole [37] LMC Udalski [34] LMC (18.36 ± 0.17) mag Cole [37] Udalski [34] Stanek [36] 15% Cole [37] I 0.6 mag 1998 Girardi [4] LMC LMC (18.28 ± 0.14) mag I I Hipparcos Udalski [34] Stanek [36] 15% 2000 Udalski [11] LMC I ( 0.6 0.2 dex) LMC ( 0.7 0.35 dex) LMC 9 [Fe/H]= 0.55 Hipparcos [Fe/H]= 0.55 LMC LMC LMC (18.24 ± 0.08) mag 2000 Romaniello [38] WFPC2 LMC SN1987A 2 (tip of red giant branch) (18.59 ± 0.04 ± 0.08) mag ( + ) ( ) (18.69 ± 0.25 ± 0.06) mag ( + ) ( TRGB) 3σ LMC 18.43 mag Romaniello [38] 2002 Alves [39] V I K LMC K LMC LMC Alves [39] LMC (18.493 ± 0.033) mag (49.96±0.77) kpc 2002 Pietrzyński Gieren [40] (ESO) LMC J K Alves [15] Hipparcos K LMC (18.487 ± 0.08 ± 0.045) mag ( + ) K 2002 Sarajedini [41] J K LMC Hodge 4 NGC
42 29 1651 K Grocholski [18] K (18.52 ± 0.17) mag (18.55 ± 0.12) mag LMC (18.54 ± 0.10) mag 2007 Grocholski [42] LMC 17 K Grocholski [42] Hipparcos LMC Grocholski Sarajedini [18] Grocholski [42] Girardi Salaris [14] LMC Girardi Salaris [14] [18] 14 LMC Grocholski [42] LMC (18.40 ± 0.04 ± 0.08) mag ( + ) R = (47.9 ± 0.9 ± 1.8) kpc Grocholski [42] Cole [37] Koerwer [43] IRSF (Infraed Survey Facility) MCPSC (Magellanic Clouds Point-Source Catalog) J H LMC H H LMC (18.54 ± 0.06) mag R = (51.1 ± 1.4) kpc Koerwer [43] (SFH) (SFR) (AMR) 2 LMC 4 K Paczyński Stanek [10] ( ) 4 (1) (2)
1 43 2 LMC /mag 1 18.08 ± 0.03 ± 0.12 1998 [34] I 2 18.065 ± 0.031 ± 0.09 1998 [36] I 3 18.36 ± 0.17 1998 [37] I 4 18.28 ± 0.14 1998 [4] I 5 18.24 ± 0.08 2000 [11] I 6 18.59 ± 0.04 ± 0.08 2000 [38] I 7 18.493 ± 0.033 2002 [39] K 8 18.487 ± 0.08 ± 0.045 2002 [40] K 9 18.54 ± 0.10 2002 [41] K 10 18.40 ± 0.04 ± 0.08 2007 [42] K 11 18.54 ± 0.06 2009 [43] H (3) (4) 4 [10] LMC SMC M31 Hipparcos 1997 10 SMC LMC M31 2012 GAIA G =15 20 20 mag 10 20 100 [44] 10% Hipparcos 100 pc [45]
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1 45 Absolute Magnitude of the Red Clump and its Applications in Distance Determination GAO Xin-hua 1,2, CHEN Li 1,3, HOU Jin-liang 1, ZHAO Jun-liang 1 (1. Key Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, Chinese Academy of Sciences, Shanghai 200030, China; 2. Graduate University of Chinese Academy of Sciences, Beijing 100049, China; 3. Key Laboratory for Research, Shanghai 200234, China) Abstract: Red clump giants are intermediate-age core helium-burning stars. Theoretical models predict that their luminosities weakly depends on their age and chemical composition. Small variance in intrinsic luminosities and weakly dependence on chemical composition and age make them an extremely useful distance indicators. Accurate parallaxes for several hundred red clump giants in the solar neighborhood provided by Hipparcos satellite have been used to estimate the mean absolute I-band and K-band magnitudes. Several I-band and K-band mean absolute magnitudes have been reported based on local red clump giants and the dependence on metallicity and color have also been investigated. Accurate distance to the Galactic center, local group and some star clusters in our Galaxy have been measured using red clump giants as reliable standard candles. By using the red clump giants population as a tracer of inner Galaxy, some researchers have analysed the structure of the bar. As all stellar distance indicators, the main worry for red clump giants lies in the possible population effects. Several studies have indicated that the luminosity dependence of the red clump giants on age and metallicity can cause significant difference in mean absolute magnitude between different stellar populations. More red clump giants with accurate parallaxes, high-quality photometry and reliable metallicities are needed to calibrate the mean absolute magnitude and the population effects. In the near future the GAIA astrometric data (position and distance), photometric data (luminosity), and spectroscopic data (metallicity, distance and extinction), will resolve this ambiguity. Key words: red clump giant; absolute magnitude; standard candle