Distance to VY Canis Majoris with VERA

Publications of the Astronomical Society of Japan

Miyaji, Takeshi^1,10  Kameya, Osamu⁶  Maruyama, Kenta¹²  Kamohara, Ryuichi^1,8  Sakai, Satoshi³  Sasao, Tetsuo⁵  Tsushima, Miyuki¹²  Manabe, Seiji⁶  Kameno, Seiji⁹  Kan-Ya, Yukitoshi⁷  Oyama, Tomoaki^1,8  Nakamura, Kayoko¹²  Iwadate, Kenzaburo³  Matsumoto, Naoko¹²  Tamura, Yoshiaki⁶  Kuji, Seisuke³  Yamashita, Kazuyoshi¹  Shibata, Katsunori M.^1,11  Omodaka, Toshihiro⁹  Nakagawa, Akiharu⁹  Kawaguchi, Noriyuki^1,11  Kim, Mi Kyoung⁴  Sato, Mayumi⁴  Bushimata, Takeshi^1,10  Matsui, Makoto¹²  Kijima, Masachika¹  Sato, Katsuhisa³  Imai, Hiroshi⁹  Kurayama, Tomoharu^1,8  Honma, Mareki¹  Oh, Chung Sik⁴  Nagayama, Takumi¹²  Jike, Takaaki³  Choi, Yoon Kyung⁴  Hirota, Tomoya¹  Kobayashi, Hideyuki² 

[1] Mizusawa VERA Observatory, National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588Department of Astronomical Sciences, Graduate University for Advanced Studies, 2-21-1 Osawa, Mitaka, Tokyo 181-8588;Department of Astronomy, Graduate School of Science, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033Mizusawa VERA Observatory, National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588Space VLBI Project, National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588Mizusawa VERA Observatory, National Astronomical Observatory of Japan, 2-12 Hoshi-ga-oka, Mizusawa-ku, Oshu-shi, Iwate 023-0861;Mizusawa VERA Observatory, National Astronomical Observatory of Japan, 2-12 Hoshi-ga-oka, Mizusawa-ku, Oshu-shi, Iwate 023-0861;Department of Astronomy, Graduate School of Science, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033Mizusawa VERA Observatory, National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588;Department of Space Survey and Information Technology, Ajou University, Suwon 443-749, Republic of KoreaKorean VLBI Network, Korea Astronomy and Space Science Institute, P.O.Box, Yonsei University, 134 Shinchon-dong, Seodaemun-gu, Seoul 120-749, Republic of Korea;Department of Astronomical Sciences, Graduate University for Advanced Studies, 2-21-1 Osawa, Mitaka, Tokyo 181-8588Mizusawa VERA Observatory, National Astronomical Observatory of Japan, 2-12 Hoshi-ga-oka, Mizusawa-ku, Oshu-shi, Iwate 023-0861;Department of Astronomy, Yonsei University, 134 Shinchon-dong, Seodaemun-gu, Seoul 120-749, Republic of Korea;Mizusawa VERA Observatory, National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588;Faculty of Science, Kagoshima University, 1-21-35 Korimoto, Kagoshima, Kagoshima 890-0065;Mizusawa VERA Observatory, National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588Space VLBI Project, National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588;Mizusawa VERA Observatory, National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588Department of Astronomical Sciences, Graduate University for Advanced Studies, 2-21-1 Osawa, Mitaka, Tokyo 181-8588Space VLBI Project, National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588;Graduate School of Science and Engineering, Kagoshima University, 1-21-35 Korimoto, Kagoshima, Kagoshima 890-0065

关键词: astrometry;    "masers (H2O)";    "stars: distances";    "stars: individual (VY Canis Majoris)";    supergiants;    VERA;   

DOI  :  10.1093/pasj/60.5.1007

学科分类：天文学(综合)

来源: Oxford University Press

【 摘 要 】

WereportonastrometricobservationsofH$$_2$$OmasersaroundtheredsupergiantVYCanisMajoriscarriedoutwithVLBIExplorationofRadioAstrometry(VERA).Basedonastrometricmonitoringfor13months,wesuccessfullymeasuredatrigonometricparallaxof0.88$$pm$$0.08mas,correspondingtoadistanceof1.14$$^{+0.11}_{-0.09}$$kpc.ThisisthemostaccuratedetermineddistancetoVYCMaandthefirstonebasedonanannualparallaxmeasurement.TheluminosityofVYCMahasbeenoverestimatedduetoapreviouslyaccepteddistance.Withourresult,were-estimatedtheluminosityofVYCMatobe(3$$pm$$0.5)$$imes$$10$$^{5}L_{odot}$$usingthebolometricfluxintegratedoveropticalandIRwavelengths.ThisimprovedluminosityvaluemakesthelocationofVYCMaontheHertzsprung-Russell(HR)diagrammuchclosertothetheoreticallyallowablezone(i.e.theleftsideoftheHayashitrack)thanpreviousones,thoughtheuncertaintyintheeffectivetemperatureofthestellarsurfacestilldoesnotpermitustomakeafinalconclusion.

【 授权许可】

Unknown