The first detection atmosphere of non-transit Neptune?

http://lyot2010.lesia.obspm.fr/abstract_131.html

Quote :

Ground-based Spectroscopic Characterization of Close-in Exoplanets
Authors

Chad Bender (1), John Carr (2), Travis Barman (3)

Affiliations

(1) PSU; (2) NRL; (3) Lowell

Abstract

We are using high-contrast, high-resolution spectroscopy from ground-based facilities to directly detect and characterize the atmospheres of close-in exoplanets. These measurements complement space-based direct detections by probing planets and spectral regions inaccessible to current space-based instruments. Observations with the NIRSPEC spectrometer on the Keck II telescope have recently yielded a direct detection of the non-transiting Neptune mass exoplanet 55 Cancri E at 3 microns. We are currently extending the program to additional targets and facilities, including the High-Resolution Spectrograph on the Hobby Eberly Telescope. I will describe our techniques for achieving very high signal-to-noise spectroscopy and the procedure for disentangling the planet and stellar spectra. I will also present our most recent results from 55 Cancri and additional systems we have been observing.

Wonder if this will also provide evidence for whether the correct orbital period of the planet is 2.817 days or 0.737 days.

Probably there were three observations.

http://adsabs.harvard.edu/abs/2008DPS....40.1108B
Two observations in 2007 and 2008.

http://nexsci.caltech.edu/missions/KeckSolicitation/proposal-current.shtml

Quote :

2009A C. Bender NRL ExP Direct Spectroscopy of Non-Transiting Exoplanets x NIRSPEC

The signal from the hot Neptune was higher than from a hot Jupiter? Although probably a variant with ultra-hot Neptune (period less than 1 day) is more like the truth.

Borislav wrote:

Probably there were three observations.

Although the text refers to 3 microns. Then the database has only two series of spectra.
https://koa.ipac.caltech.edu/cgi-bin/KOA/nph-KOAlogin

2007-12-11 14:13:29.05 - 2007-12-11 16:09:48.50
2007-12-13 14:46:39.80 - 2007-12-13 16:25:00.86

The difference between the observations about 48 hours.

For both periods, we obtain a good phase differences:
0.737 days - 2.8
2.817 days - 1.4

If I understood well the weak period is confirmed. Then in spite of temperature extremes on this planet, she is like Neptune?

Stalker wrote:

If I understood well the weak period is confirmed. Then in spite of temperature extremes on this planet, she is like Neptune?

m sin i = 8,3 mEarth
http://iopscience.iop.org/1538-4357/614/1/L81/18785.text.html
If the orbits are coplanar, then about 10 Earth masses.

http://arxiv.org/pdf/1005.4050v3

Quote :

Third, even apart from a transit, this super-Earth must be very hot, as it is very close-in to a solar-type star. Following L´eger et al. (2009), we find that the substellar point could be up to 2750 K, if the insolation is absorbed then reradiated locally. We would naively expect that the enormous radiation this planet takes in would evaporate any atmosphere (e.g., Jackson et al. 2010). Moreover, the host star is also very bright as seen from Earth. Therefore it might be useful to look for its phase curve with Spitzer, to detect or rule out an atmosphere (Seager & Deming 2009). Another attractive possibility is probing a magma ocean, which may exist because of the irradiation (Gelman et al. 2009; Gaidos et al. 2010), but this may require transit measurements.
Fourth, the presence of the other 4 planets surely injects a non-zero eccentricity into this tidally-dissipating planet. Its expected value remains to be calculated, but will likely be on the order of 10−4. This forced eccentricity could stimulate considerable geologic activity — it might be a “super-Io” (Barnes et al. 2010).

But now found another abstract by January 2010
http://adsabs.harvard.edu/abs/2010AAS...21542121B

And at that time period has not yet been reviewed ...