HAT-P-32b and HAT-P-33b

Two highly inflated hot Jupiters transiting high-jitter stars

J. D. Hartman, G. Á Bakos, G. Torres, D. W. Latham, Géza Kovács, B. Béky, S. N. Quinn, T. Mazeh, A. Shporer, G. W. Marcy, A. W. Howard, D. A. Fischer, J. A. Johnson, G. A. Esquerdo, R. W. Noyes, D. D. Sasselov, R. P. Stefanik, J. M. Fernandez, T. Szklenár, J. Lázár & 2 others I. Papp, P. Sári

Research output: Contribution to journalArticle

81 Citations (Scopus)

Abstract

We report the discovery of two exoplanets transiting high-jitter stars. HAT-P-32b orbits the bright V = 11.289 late-F-early-G dwarf star GSC 3281-00800, with a period P = 2.150008 ± 0.000001d. The stellar and planetary masses and radii depend on the eccentricity of the system, which is poorly constrained due to the high-velocity jitter (∼80 m s-1). Assuming a circular orbit, the star has a mass of 1.16±0.04 M Ȯ and radius of 1.22±0.02 R Ȯ, while the planet has a mass of 0.860±0.164 M J and a radius of 1.789 0.025R J. The second planet, HAT-P-33b, orbits the bright V = 11.188 late-F dwarf star GSC 2461-00988, with a period P = 3.474474±0.000001d. As for HAT-P-32, the stellar and planetary masses and radii of HAT-P-33 depend on the eccentricity, which is poorly constrained due to the high jitter (∼50 m s-1). In this case, spectral line bisector spans (BSs) are significantly anti-correlated with the radial velocity residuals, and we are able to use this correlation to reduce the residual rms to ∼35 m s-1. We find that the star has a mass of 1.38±0.04 M Ȯ and a radius of 1.64±0.03 R Ȯ while the planet has a mass of 0.762 0.101 M J and a radius of 1.686±0.045R J for an assumed circular orbit. Due to the large BS variations exhibited by both stars we rely on detailed modeling of the photometric light curves to rule out blend scenarios. Both planets are among the largest radii transiting planets discovered to date.

Original languageEnglish
Article number59
JournalAstrophysical Journal
Volume742
Issue number1
DOIs
Publication statusPublished - Nov 20 2011

Fingerprint

Jupiter (planet)
Jupiter
planet
stars
vibration
planets
radii
planetary mass
dwarf stars
eccentricity
circular orbits
stellar mass
G stars
F stars
orbits
extrasolar planets
radial velocity
light curve
line spectra
modeling

Keywords

  • planetary systems
  • stars: individual (HAT-P-32, GSC 3281-00800, HAT-P-33, GSC 2461-00988)
  • techniques: photometric
  • techniques: spectroscopic

ASJC Scopus subject areas

  • Nuclear and High Energy Physics
  • Space and Planetary Science
  • Astronomy and Astrophysics

Cite this

HAT-P-32b and HAT-P-33b : Two highly inflated hot Jupiters transiting high-jitter stars. / Hartman, J. D.; Bakos, G. Á; Torres, G.; Latham, D. W.; Kovács, Géza; Béky, B.; Quinn, S. N.; Mazeh, T.; Shporer, A.; Marcy, G. W.; Howard, A. W.; Fischer, D. A.; Johnson, J. A.; Esquerdo, G. A.; Noyes, R. W.; Sasselov, D. D.; Stefanik, R. P.; Fernandez, J. M.; Szklenár, T.; Lázár, J.; Papp, I.; Sári, P.

In: Astrophysical Journal, Vol. 742, No. 1, 59, 20.11.2011.

Research output: Contribution to journalArticle

Hartman, JD, Bakos, GÁ, Torres, G, Latham, DW, Kovács, G, Béky, B, Quinn, SN, Mazeh, T, Shporer, A, Marcy, GW, Howard, AW, Fischer, DA, Johnson, JA, Esquerdo, GA, Noyes, RW, Sasselov, DD, Stefanik, RP, Fernandez, JM, Szklenár, T, Lázár, J, Papp, I & Sári, P 2011, 'HAT-P-32b and HAT-P-33b: Two highly inflated hot Jupiters transiting high-jitter stars', Astrophysical Journal, vol. 742, no. 1, 59. https://doi.org/10.1088/0004-637X/742/1/59
Hartman, J. D. ; Bakos, G. Á ; Torres, G. ; Latham, D. W. ; Kovács, Géza ; Béky, B. ; Quinn, S. N. ; Mazeh, T. ; Shporer, A. ; Marcy, G. W. ; Howard, A. W. ; Fischer, D. A. ; Johnson, J. A. ; Esquerdo, G. A. ; Noyes, R. W. ; Sasselov, D. D. ; Stefanik, R. P. ; Fernandez, J. M. ; Szklenár, T. ; Lázár, J. ; Papp, I. ; Sári, P. / HAT-P-32b and HAT-P-33b : Two highly inflated hot Jupiters transiting high-jitter stars. In: Astrophysical Journal. 2011 ; Vol. 742, No. 1.
@article{7b79e1c792b047d68a689ecef32b8f2b,
title = "HAT-P-32b and HAT-P-33b: Two highly inflated hot Jupiters transiting high-jitter stars",
abstract = "We report the discovery of two exoplanets transiting high-jitter stars. HAT-P-32b orbits the bright V = 11.289 late-F-early-G dwarf star GSC 3281-00800, with a period P = 2.150008 ± 0.000001d. The stellar and planetary masses and radii depend on the eccentricity of the system, which is poorly constrained due to the high-velocity jitter (∼80 m s-1). Assuming a circular orbit, the star has a mass of 1.16±0.04 M Ȯ and radius of 1.22±0.02 R Ȯ, while the planet has a mass of 0.860±0.164 M J and a radius of 1.789 0.025R J. The second planet, HAT-P-33b, orbits the bright V = 11.188 late-F dwarf star GSC 2461-00988, with a period P = 3.474474±0.000001d. As for HAT-P-32, the stellar and planetary masses and radii of HAT-P-33 depend on the eccentricity, which is poorly constrained due to the high jitter (∼50 m s-1). In this case, spectral line bisector spans (BSs) are significantly anti-correlated with the radial velocity residuals, and we are able to use this correlation to reduce the residual rms to ∼35 m s-1. We find that the star has a mass of 1.38±0.04 M Ȯ and a radius of 1.64±0.03 R Ȯ while the planet has a mass of 0.762 0.101 M J and a radius of 1.686±0.045R J for an assumed circular orbit. Due to the large BS variations exhibited by both stars we rely on detailed modeling of the photometric light curves to rule out blend scenarios. Both planets are among the largest radii transiting planets discovered to date.",
keywords = "planetary systems, stars: individual (HAT-P-32, GSC 3281-00800, HAT-P-33, GSC 2461-00988), techniques: photometric, techniques: spectroscopic",
author = "Hartman, {J. D.} and Bakos, {G. {\'A}} and G. Torres and Latham, {D. W.} and G{\'e}za Kov{\'a}cs and B. B{\'e}ky and Quinn, {S. N.} and T. Mazeh and A. Shporer and Marcy, {G. W.} and Howard, {A. W.} and Fischer, {D. A.} and Johnson, {J. A.} and Esquerdo, {G. A.} and Noyes, {R. W.} and Sasselov, {D. D.} and Stefanik, {R. P.} and Fernandez, {J. M.} and T. Szklen{\'a}r and J. L{\'a}z{\'a}r and I. Papp and P. S{\'a}ri",
year = "2011",
month = "11",
day = "20",
doi = "10.1088/0004-637X/742/1/59",
language = "English",
volume = "742",
journal = "Astrophysical Journal",
issn = "0004-637X",
publisher = "IOP Publishing Ltd.",
number = "1",

}

TY - JOUR

T1 - HAT-P-32b and HAT-P-33b

T2 - Two highly inflated hot Jupiters transiting high-jitter stars

AU - Hartman, J. D.

AU - Bakos, G. Á

AU - Torres, G.

AU - Latham, D. W.

AU - Kovács, Géza

AU - Béky, B.

AU - Quinn, S. N.

AU - Mazeh, T.

AU - Shporer, A.

AU - Marcy, G. W.

AU - Howard, A. W.

AU - Fischer, D. A.

AU - Johnson, J. A.

AU - Esquerdo, G. A.

AU - Noyes, R. W.

AU - Sasselov, D. D.

AU - Stefanik, R. P.

AU - Fernandez, J. M.

AU - Szklenár, T.

AU - Lázár, J.

AU - Papp, I.

AU - Sári, P.

PY - 2011/11/20

Y1 - 2011/11/20

N2 - We report the discovery of two exoplanets transiting high-jitter stars. HAT-P-32b orbits the bright V = 11.289 late-F-early-G dwarf star GSC 3281-00800, with a period P = 2.150008 ± 0.000001d. The stellar and planetary masses and radii depend on the eccentricity of the system, which is poorly constrained due to the high-velocity jitter (∼80 m s-1). Assuming a circular orbit, the star has a mass of 1.16±0.04 M Ȯ and radius of 1.22±0.02 R Ȯ, while the planet has a mass of 0.860±0.164 M J and a radius of 1.789 0.025R J. The second planet, HAT-P-33b, orbits the bright V = 11.188 late-F dwarf star GSC 2461-00988, with a period P = 3.474474±0.000001d. As for HAT-P-32, the stellar and planetary masses and radii of HAT-P-33 depend on the eccentricity, which is poorly constrained due to the high jitter (∼50 m s-1). In this case, spectral line bisector spans (BSs) are significantly anti-correlated with the radial velocity residuals, and we are able to use this correlation to reduce the residual rms to ∼35 m s-1. We find that the star has a mass of 1.38±0.04 M Ȯ and a radius of 1.64±0.03 R Ȯ while the planet has a mass of 0.762 0.101 M J and a radius of 1.686±0.045R J for an assumed circular orbit. Due to the large BS variations exhibited by both stars we rely on detailed modeling of the photometric light curves to rule out blend scenarios. Both planets are among the largest radii transiting planets discovered to date.

AB - We report the discovery of two exoplanets transiting high-jitter stars. HAT-P-32b orbits the bright V = 11.289 late-F-early-G dwarf star GSC 3281-00800, with a period P = 2.150008 ± 0.000001d. The stellar and planetary masses and radii depend on the eccentricity of the system, which is poorly constrained due to the high-velocity jitter (∼80 m s-1). Assuming a circular orbit, the star has a mass of 1.16±0.04 M Ȯ and radius of 1.22±0.02 R Ȯ, while the planet has a mass of 0.860±0.164 M J and a radius of 1.789 0.025R J. The second planet, HAT-P-33b, orbits the bright V = 11.188 late-F dwarf star GSC 2461-00988, with a period P = 3.474474±0.000001d. As for HAT-P-32, the stellar and planetary masses and radii of HAT-P-33 depend on the eccentricity, which is poorly constrained due to the high jitter (∼50 m s-1). In this case, spectral line bisector spans (BSs) are significantly anti-correlated with the radial velocity residuals, and we are able to use this correlation to reduce the residual rms to ∼35 m s-1. We find that the star has a mass of 1.38±0.04 M Ȯ and a radius of 1.64±0.03 R Ȯ while the planet has a mass of 0.762 0.101 M J and a radius of 1.686±0.045R J for an assumed circular orbit. Due to the large BS variations exhibited by both stars we rely on detailed modeling of the photometric light curves to rule out blend scenarios. Both planets are among the largest radii transiting planets discovered to date.

KW - planetary systems

KW - stars: individual (HAT-P-32, GSC 3281-00800, HAT-P-33, GSC 2461-00988)

KW - techniques: photometric

KW - techniques: spectroscopic

UR - http://www.scopus.com/inward/record.url?scp=80755169587&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=80755169587&partnerID=8YFLogxK

U2 - 10.1088/0004-637X/742/1/59

DO - 10.1088/0004-637X/742/1/59

M3 - Article

VL - 742

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 1

M1 - 59

ER -