OGLE-2005-BLG-071Lb, the most massive M dwarf planetary companion?

Dong, S; Gould, A; Udalski, A; Anderson, J; Christie, GW; Gaudi, BS; Jaroszynski, M; Kubiak, M; Szymanski, MK; Pietrzynski, G; Soszynski, I; Szewczyk, O; Ulaczyk, K; Wyrzykowski, L; DePoy, DL; Fox, DB; Gal-Yam, A; Han, C; Lepine, S; McCormick, J; Ofek, E; Park, BG; Pogge, RW; Abe, F; Bennett, DP; Bond, IA; Britton, TR; Gilmore, AC; Hearnshaw, JB; Itow, Y; Kamiya, K; Kilmartin, PM; Korpela, A; Masuda, K; Matsubara, Y; Motomura, M; Muraki, Y; Nakamura, S; Ohnishi, K; Okada, C; Rattenbury, N; Saito, T; Sako, T; Sasaki, M; Sullivan, D; Sumi, T; Tristram, PJ; Yanagisawa, T; Yock, PMC; Yoshoika, T; Albrow, MD; Beaulieu, JP; Brilliant, S; Calitz, H; Cassan, A; Cook, KH; Coutures, C; Dieters, S; Dominis Prester, D; Donatowicz, J; Fouque, P; Greenhill, JG; Hill, KM; Hoffman, M; Horne, K; Jorgensen, UG; Kane, S; Kubas, D; Marquette, JB; Martin, R; Meintjes, P; Menzies, J; Pollard, KR; Sahu, KC; Vinter, C; Wambsganss, J; Williams, A; Bode, M; Bramich, DM; Burgdorf, M; Snodgrass, C; Steele, I; Doublier, V; Foellmi, C

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OGLE-2005-BLG-071Lb, the most massive M dwarf planetary companion?

Citation

Dong, S and Gould, A and Udalski, A and Anderson, J and Christie, GW and Gaudi, BS and Jaroszynski, M and Kubiak, M and Szymanski, MK and Pietrzynski, G and Soszynski, I and Szewczyk, O and Ulaczyk, K and Wyrzykowski, L and DePoy, DL and Fox, DB and Gal-Yam, A and Han, C and Lepine, S and McCormick, J and Ofek, E and Park, BG and Pogge, RW and Abe, F and Bennett, DP and Bond, IA and Britton, TR and Gilmore, AC and Hearnshaw, JB and Itow, Y and Kamiya, K and Kilmartin, PM and Korpela, A and Masuda, K and Matsubara, Y and Motomura, M and Muraki, Y and Nakamura, S and Ohnishi, K and Okada, C and Rattenbury, N and Saito, T and Sako, T and Sasaki, M and Sullivan, D and Sumi, T and Tristram, PJ and Yanagisawa, T and Yock, PMC and Yoshoika, T and Albrow, MD and Beaulieu, JP and Brilliant, S and Calitz, H and Cassan, A and Cook, KH and Coutures, C and Dieters, S and Dominis Prester, D and Donatowicz, J and Fouque, P and Greenhill, JG and Hill, KM and Hoffman, M and Horne, K and Jorgensen, UG and Kane, S and Kubas, D and Marquette, JB and Martin, R and Meintjes, P and Menzies, J and Pollard, KR and Sahu, KC and Vinter, C and Wambsganss, J and Williams, A and Bode, M and Bramich, DM and Burgdorf, M and Snodgrass, C and Steele, I and Doublier, V and Foellmi, C, OGLE-2005-BLG-071Lb, the most massive M dwarf planetary companion?, The Astrophysical Journal, 695, (2) pp. 970-987. ISSN 0004-637X (2009) [Refereed Article]

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Official URL: http://aas.org/

DOI: doi:10.1088/0004-637X/695/2/970

Abstract

We combine all available information to constrain the nature of OGLE-2005-BLG-071Lb, the second planet discovered by microlensing and the first in a high-magnification event. These include photometric and astrometric measurements from the Hubble Space Telescope, as well as constraints from higher order effects extracted from the ground-based light curve, such as microlens parallax, planetary orbital motion, and finite-source effects. Our primary analysis leads to the conclusion that the host of Jovian planet OGLE-2005-BLG-071Lb is an M dwarf in the foreground disk with mass M = 0.46 ± 0.04 M_☉, distance D_l = 3.2 ± 0.4 kpc, and thick-disk kinematics v_LSR ∼ 103 km s⁻¹. From the best-fit model, the planet has mass M_p = 3.8 ± 0.4 M_Jupiter, lies at a projected separation r_⊥ = 3.6 ± 0.2AU from its host, and so has an equilibrium temperature of T ∼ 55 K, that is, similar to Neptune. A degenerate model gives similar planetary mass M_p = 3.4 ± 0.4 M_Jupiter with a smaller projected separation, r_⊥ = 2.1 ± 0.1AU, and higher equilibrium temperature, T ∼ 71 K. These results from the primary analysis suggest that OGLE-2005-BLG-071Lb is likely to be the most massive planet yet discovered that is hosted by an M dwarf. However, the formation of such high-mass planetary companions in the outer regions of M dwarf planetary systems is predicted to be unlikely within the core-accretion scenario. There are a number of caveats to this primary analysis, which assumes (based on real but limited evidence) that the unlensed light coincident with the source is actually due to the lens, that is, the planetary host. However, these caveats could mostly be resolved by a single astrometric measurement a few years after the event.

Item Details

Item Type:	Refereed Article
Keywords:	galaxy;bulge-gravitational lensing-planetary systems
Research Division:	Physical Sciences
Research Group:	Astronomical sciences
Research Field:	Galactic astronomy
Objective Division:	Expanding Knowledge
Objective Group:	Expanding knowledge
Objective Field:	Expanding knowledge in the physical sciences
UTAS Author:	Beaulieu, JP (Dr Jean-Philippe Beaulieu)
UTAS Author:	Dieters, S (Dr Stefan Dieters)
UTAS Author:	Greenhill, JG (Dr John Greenhill)
UTAS Author:	Hill, KM (Dr Kym Hill)
ID Code:	57591
Year Published:	2009
Web of Science^® Times Cited:	130
Deposited By:	Physics
Deposited On:	2009-07-28
Last Modified:	2022-07-13
Downloads:	0

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