D. P. Mahtani
Current Organizations / Institutes
The organizations/institutes from the scholar's latest article
Research Subjects
Research Interests
D. P. Mahtani has a total of 27 co-authors. Here are the top co-authors by number of shared publications:
J. Southworth
Astrophysics Group, Keele University, Keele, Staffordshire, ST5 5BG, UK
2 shared publicationsJ. Tregloan-Reed
Astrophysics Group, Keele University, Keele, Staffordshire, ST5 5BG, UK
2 shared publicationsN. Madhusudhan
Department of Physics and Department of Astronomy, Yale University, New Haven, CT 06520-8101, USA
2 shared publicationsA. Collier Cameron
SUPA School of Physics and Astronomy University of St. Andrews North Haugh KY16 9SS Fife
1 shared publicationA. H. M. J. Triaud
Université de Genève 51 ch. des Maillettes 1290 Sauverny Switzerland
1 shared publicationA. M. S. Smith
Astrophysics Group Keele University Staffordshire ST5 5BG
1 shared publication
Latest Publications
- Open Access
- 17 April 2013
- Published by Oxford University Press (OUP) in Monthly Notices of the Royal Astronomical Society
- Vol. 432 (1) , 693-701
Warm Spitzer occultation photometry of WASP-26b at 3.6 and 4.5 μm
We present new warm Spitzer occultation photometry of WASP-26 at 3.6 and 4.5 μm along with new transit photometry taken in the g, r and i bands. We report the first detection of the occultation of WASP-26b, with occultation depths at 3.6 and 4.5 μm of 0.001 26 ± 0.000 13 and 0.001 49 ± 0.000 16 corresponding to brightness temperatures of 1825 ± 80 and 1725 ± 89 K, respectively. We find that the eccentricity of the orbit is consistent with a circular orbit at the 1σ level ($$e=0.0028 ^{+ 0.0097}_{- 0.0022}$$, 3σ upper limit e < 0.04). According to the activity–inversion relation of Knutson et al., WASP-26b is predicted to host a thermal inversion. The brightness temperatures deduced from the eclipse depths are consistent with an isothermal atmosphere, although the planet may host a weak thermal inversion given the uncertainties on these values. The data are equally well fitted by atmospheric models with or without a thermal inversion. We find that variation in activity of solar-like stars does not change enough over the time-scales of months or years to change the interpretation of the Knutson et al. activity–inversion relation, provided that the measured activity level is averaged over several nights. Further data are required to fully constrain the thermal structure of the atmosphere because the planet lies very close to the boundary between atmospheres with and without a thermal inversion.- 17 April 2013
- Published by Oxford University Press (OUP) in Monthly Notices of the Royal Astronomical Society
- Vol. 432 (1) , 693-701
Open AccessWarm Spitzer occultation photometry of WASP-26b at 3.6 and 4.5 μm
We present new warm Spitzer occultation photometry of WASP-26 at 3.6 and 4.5 μm along with new transit photometry taken in the g, r and i bands. We report the first detection of the occultation of WASP-26b, with occultation depths at 3.6 and 4.5 μm of 0.001 26 ± 0.000 13 and 0.001 49 ± 0.000 16 corresponding to brightness temperatures of 1825 ± 80 and 1725 ± 89 K, respectively. We find that the eccentricity of the orbit is consistent with a circular orbit at the 1σ level ($$e=0.0028 ^{+ 0.0097}_{- 0.0022}$$, 3σ upper limit e < 0.04). According to the activity–inversion relation of Knutson et al., WASP-26b is predicted to host a thermal inversion. The brightness temperatures deduced from the eclipse depths are consistent with an isothermal atmosphere, although the planet may host a weak thermal inversion given the uncertainties on these values. The data are equally well fitted by atmospheric models with or without a thermal inversion. We find that variation in activity of solar-like stars does not change enough over the time-scales of months or years to change the interpretation of the Knutson et al. activity–inversion relation, provided that the measured activity level is averaged over several nights. Further data are required to fully constrain the thermal structure of the atmosphere because the planet lies very close to the boundary between atmospheres with and without a thermal inversion. - Open Access
Warm Spitzer Occultation Photometry of WASP-26b at 3.6μm and 4.5μm
We present new warm Spitzer occultation photometry of WASP-26 at 3.6{\mu}m and 4.5{\mu}m along with new transit photometry taken in the g,r and i bands. We report the first detection of the occultation of WASP-26b, with occultation depths at 3.6{\mu}m and 4.5{\mu}m of 0.00126 +/- 0.00013 and 0.00149 +/- 0.00016 corresponding to brightness temperatures of 1825+/-80K and 1725+/-89K, respectively. We find that the eccentricity of the orbit is consistent with a circular orbit at the 1{\sigma} level with a 3{\sigma} upper limit of e < 0.04. According to the activity-inversion relation of Knutson et al. (2010), WASP-26b is predicted to host a thermal inversion. The brightness temperatures deduced from the eclipse depths are consistent with an isothermal atmosphere, although it is within the uncertainties that the planet may host a weak thermal inversion. The data are equally well fit by atmospheric models with or without a thermal inversion. We find that variation in activity of solar-like stars does not change enough over the time-scales of months or years to change the interpretation of the Knutson et al. (2010) activity-inversion relation, provided that the measured activity level is averaged over several nights. Further data are required to fully constrain the thermal structure of the atmosphere because the planet lies very close to the boundary between atmospheres with and without a thermal inversion.
Open AccessWarm Spitzer Occultation Photometry of WASP-26b at 3.6μm and 4.5μm
We present new warm Spitzer occultation photometry of WASP-26 at 3.6{\mu}m and 4.5{\mu}m along with new transit photometry taken in the g,r and i bands. We report the first detection of the occultation of WASP-26b, with occultation depths at 3.6{\mu}m and 4.5{\mu}m of 0.00126 +/- 0.00013 and 0.00149 +/- 0.00016 corresponding to brightness temperatures of 1825+/-80K and 1725+/-89K, respectively. We find that the eccentricity of the orbit is consistent with a circular orbit at the 1{\sigma} level with a 3{\sigma} upper limit of e < 0.04. According to the activity-inversion relation of Knutson et al. (2010), WASP-26b is predicted to host a thermal inversion. The brightness temperatures deduced from the eclipse depths are consistent with an isothermal atmosphere, although it is within the uncertainties that the planet may host a weak thermal inversion. The data are equally well fit by atmospheric models with or without a thermal inversion. We find that variation in activity of solar-like stars does not change enough over the time-scales of months or years to change the interpretation of the Knutson et al. (2010) activity-inversion relation, provided that the measured activity level is averaged over several nights. Further data are required to fully constrain the thermal structure of the atmosphere because the planet lies very close to the boundary between atmospheres with and without a thermal inversion.