Warm Spitzer photometry of three hot Jupiters: HAT-P-3b, HAT-P-4b and HAT-P-12b

Kamen O. Todorov, Drake Deming, Heather A. Knutson, Adam Burrows, Jonathan J. Fortney, Nikole K. Lewis, Nicolas B. Cowan, Eric Agol, Jean Michel Desert, Pedro V. Sada, David Charbonneau, Gregory Laughlin, Jonathan Langton, Adam P. Showman

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Abstract

We present Warm Spitzer/IRAC secondary eclipse time series photometry of three short-period transiting exoplanets, HAT-P-3b, HAT-P-4b and HAT-P-12b, in both the available 3.6 and 4.5 μm bands. HAT-P-3b and HAT-P-4b are Jupiter-mass objects orbiting an early K and an early G dwarf star, respectively. For HAT-P-3b we find eclipse depths of (3.6 μm) and (4.5 μm). The HAT-P-4b values are (3.6 μm) and (4.5 μm). The two planets' photometry is consistent with inefficient heat redistribution from their day to night sides (and low albedos), but it is inconclusive about possible temperature inversions in their atmospheres. HAT-P-12b is a Saturn-mass planet and is one of the coolest planets ever observed during secondary eclipse, along with the hot Neptune GJ 436b and the hot Saturn WASP-29b. We are able to place 3σ upper limits on the secondary eclipse depth of HAT-P-12b in both wavelengths: <0.042% (3.6 μm) and <0.085% (4.5 μm). We discuss these results in the context of the Spitzer secondary eclipse measurements of GJ 436b and WASP-29b. It is possible that we do not detect the eclipses of HAT-P-12b due to high eccentricity, but find that weak planetary emission in these wavelengths is a more likely explanation. We place 3σ upper limits on the |e cos ω| quantity (where e is eccentricity and ω is the argument of periapsis) for HAT-P-3b (<0.0081) and HAT-P-4b (<0.0042), based on the secondary eclipse timings. © 2013. The American Astronomical Society. All rights reserved..
Original languageEnglish
JournalAstrophysical Journal
DOIs
Publication statusPublished - 20 Jun 2013

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eclipses
Jupiter (planet)
Jupiter
photometry
planet
Saturn
eccentricity
wavelength
temperature inversion
Neptune
planets
albedo
time series
G stars
atmosphere
temperature inversions
dwarf stars
Neptune (planet)
extrasolar planets
wavelengths

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Todorov, K. O., Deming, D., Knutson, H. A., Burrows, A., Fortney, J. J., Lewis, N. K., ... Showman, A. P. (2013). Warm Spitzer photometry of three hot Jupiters: HAT-P-3b, HAT-P-4b and HAT-P-12b. Astrophysical Journal. https://doi.org/10.1088/0004-637X/770/2/102
Todorov, Kamen O. ; Deming, Drake ; Knutson, Heather A. ; Burrows, Adam ; Fortney, Jonathan J. ; Lewis, Nikole K. ; Cowan, Nicolas B. ; Agol, Eric ; Desert, Jean Michel ; Sada, Pedro V. ; Charbonneau, David ; Laughlin, Gregory ; Langton, Jonathan ; Showman, Adam P. / Warm Spitzer photometry of three hot Jupiters: HAT-P-3b, HAT-P-4b and HAT-P-12b. In: Astrophysical Journal. 2013.
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title = "Warm Spitzer photometry of three hot Jupiters: HAT-P-3b, HAT-P-4b and HAT-P-12b",
abstract = "We present Warm Spitzer/IRAC secondary eclipse time series photometry of three short-period transiting exoplanets, HAT-P-3b, HAT-P-4b and HAT-P-12b, in both the available 3.6 and 4.5 μm bands. HAT-P-3b and HAT-P-4b are Jupiter-mass objects orbiting an early K and an early G dwarf star, respectively. For HAT-P-3b we find eclipse depths of (3.6 μm) and (4.5 μm). The HAT-P-4b values are (3.6 μm) and (4.5 μm). The two planets' photometry is consistent with inefficient heat redistribution from their day to night sides (and low albedos), but it is inconclusive about possible temperature inversions in their atmospheres. HAT-P-12b is a Saturn-mass planet and is one of the coolest planets ever observed during secondary eclipse, along with the hot Neptune GJ 436b and the hot Saturn WASP-29b. We are able to place 3σ upper limits on the secondary eclipse depth of HAT-P-12b in both wavelengths: <0.042{\%} (3.6 μm) and <0.085{\%} (4.5 μm). We discuss these results in the context of the Spitzer secondary eclipse measurements of GJ 436b and WASP-29b. It is possible that we do not detect the eclipses of HAT-P-12b due to high eccentricity, but find that weak planetary emission in these wavelengths is a more likely explanation. We place 3σ upper limits on the |e cos ω| quantity (where e is eccentricity and ω is the argument of periapsis) for HAT-P-3b (<0.0081) and HAT-P-4b (<0.0042), based on the secondary eclipse timings. {\circledC} 2013. The American Astronomical Society. All rights reserved..",
author = "Todorov, {Kamen O.} and Drake Deming and Knutson, {Heather A.} and Adam Burrows and Fortney, {Jonathan J.} and Lewis, {Nikole K.} and Cowan, {Nicolas B.} and Eric Agol and Desert, {Jean Michel} and Sada, {Pedro V.} and David Charbonneau and Gregory Laughlin and Jonathan Langton and Showman, {Adam P.}",
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month = "6",
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Todorov, KO, Deming, D, Knutson, HA, Burrows, A, Fortney, JJ, Lewis, NK, Cowan, NB, Agol, E, Desert, JM, Sada, PV, Charbonneau, D, Laughlin, G, Langton, J & Showman, AP 2013, 'Warm Spitzer photometry of three hot Jupiters: HAT-P-3b, HAT-P-4b and HAT-P-12b', Astrophysical Journal. https://doi.org/10.1088/0004-637X/770/2/102

Warm Spitzer photometry of three hot Jupiters: HAT-P-3b, HAT-P-4b and HAT-P-12b. / Todorov, Kamen O.; Deming, Drake; Knutson, Heather A.; Burrows, Adam; Fortney, Jonathan J.; Lewis, Nikole K.; Cowan, Nicolas B.; Agol, Eric; Desert, Jean Michel; Sada, Pedro V.; Charbonneau, David; Laughlin, Gregory; Langton, Jonathan; Showman, Adam P.

In: Astrophysical Journal, 20.06.2013.

Research output: Contribution to journalArticle

TY - JOUR

T1 - Warm Spitzer photometry of three hot Jupiters: HAT-P-3b, HAT-P-4b and HAT-P-12b

AU - Todorov, Kamen O.

AU - Deming, Drake

AU - Knutson, Heather A.

AU - Burrows, Adam

AU - Fortney, Jonathan J.

AU - Lewis, Nikole K.

AU - Cowan, Nicolas B.

AU - Agol, Eric

AU - Desert, Jean Michel

AU - Sada, Pedro V.

AU - Charbonneau, David

AU - Laughlin, Gregory

AU - Langton, Jonathan

AU - Showman, Adam P.

PY - 2013/6/20

Y1 - 2013/6/20

N2 - We present Warm Spitzer/IRAC secondary eclipse time series photometry of three short-period transiting exoplanets, HAT-P-3b, HAT-P-4b and HAT-P-12b, in both the available 3.6 and 4.5 μm bands. HAT-P-3b and HAT-P-4b are Jupiter-mass objects orbiting an early K and an early G dwarf star, respectively. For HAT-P-3b we find eclipse depths of (3.6 μm) and (4.5 μm). The HAT-P-4b values are (3.6 μm) and (4.5 μm). The two planets' photometry is consistent with inefficient heat redistribution from their day to night sides (and low albedos), but it is inconclusive about possible temperature inversions in their atmospheres. HAT-P-12b is a Saturn-mass planet and is one of the coolest planets ever observed during secondary eclipse, along with the hot Neptune GJ 436b and the hot Saturn WASP-29b. We are able to place 3σ upper limits on the secondary eclipse depth of HAT-P-12b in both wavelengths: <0.042% (3.6 μm) and <0.085% (4.5 μm). We discuss these results in the context of the Spitzer secondary eclipse measurements of GJ 436b and WASP-29b. It is possible that we do not detect the eclipses of HAT-P-12b due to high eccentricity, but find that weak planetary emission in these wavelengths is a more likely explanation. We place 3σ upper limits on the |e cos ω| quantity (where e is eccentricity and ω is the argument of periapsis) for HAT-P-3b (<0.0081) and HAT-P-4b (<0.0042), based on the secondary eclipse timings. © 2013. The American Astronomical Society. All rights reserved..

AB - We present Warm Spitzer/IRAC secondary eclipse time series photometry of three short-period transiting exoplanets, HAT-P-3b, HAT-P-4b and HAT-P-12b, in both the available 3.6 and 4.5 μm bands. HAT-P-3b and HAT-P-4b are Jupiter-mass objects orbiting an early K and an early G dwarf star, respectively. For HAT-P-3b we find eclipse depths of (3.6 μm) and (4.5 μm). The HAT-P-4b values are (3.6 μm) and (4.5 μm). The two planets' photometry is consistent with inefficient heat redistribution from their day to night sides (and low albedos), but it is inconclusive about possible temperature inversions in their atmospheres. HAT-P-12b is a Saturn-mass planet and is one of the coolest planets ever observed during secondary eclipse, along with the hot Neptune GJ 436b and the hot Saturn WASP-29b. We are able to place 3σ upper limits on the secondary eclipse depth of HAT-P-12b in both wavelengths: <0.042% (3.6 μm) and <0.085% (4.5 μm). We discuss these results in the context of the Spitzer secondary eclipse measurements of GJ 436b and WASP-29b. It is possible that we do not detect the eclipses of HAT-P-12b due to high eccentricity, but find that weak planetary emission in these wavelengths is a more likely explanation. We place 3σ upper limits on the |e cos ω| quantity (where e is eccentricity and ω is the argument of periapsis) for HAT-P-3b (<0.0081) and HAT-P-4b (<0.0042), based on the secondary eclipse timings. © 2013. The American Astronomical Society. All rights reserved..

U2 - 10.1088/0004-637X/770/2/102

DO - 10.1088/0004-637X/770/2/102

M3 - Article

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

ER -