Revisiting HST/COS Transit Observations in the FUV of Hot Jupiters

Details Revisiting HST/COS Transit Observations in the FUV of Hot Jupiters Revisiting HST/COS Transit Observations in the FUV of Hot Jupiters

Sep 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011ess.....2.4026b&link_type=abstract

American Astronomical Society, ESS meeting #2, #40.26

Astronomy and Astrophysics

Astronomy

Scientific paper

One transit of the hot Jupiter HD 209458b was observed in the FUV with
the COS instrument using the G130M grating by Linsky et al. (Ap. J.,
717, 1291, 2010). The data were averaged over the single HST orbit,
and then contrasted against an average spectrum of the star obtained at
different dates (with the planet off-transit). A positive detection of
absorption (7.8% +/- 1.3%) by extended CII ions (at 1335 Ang) was
reported confirming that from previous HST/STIS observations (7.8% +/-
3.5%; Vidal-Madjar et al., Ap. J. 604, L69, 2004; 7.4% +/- 4.7%
Ben-Jaffel and Hosseini (Ap. J., 709, 1289, 2010) and showing
absorption excess in the blue line-wings, indicative of a tail of
escaping C+ ions. Linsky et al. also reported a positive detection of
Si III ions (8.2% +/- 1.4% at 1206 Ang). In contrast, the previous
STIS observations did not show a transit absorption signature in Si III
(1206 Ang), and, furthermore, they showed variations at the few percent
level in both the C II and Si III stellar emissions. The transit
results of Linsky et al. could thus be associated with stellar
variation.
Here, we will use the time-tagging of the COS data to determine the
true transit absorption signature by resolving mid-transit against
egress behavior (transit light curves) sampled during the HST orbit.
We will also evaluate a COS G130M observations of HD 189733 which,
unfortunately, only covered the egress portion of its hot Jupiter
transit (as well as consecutive HST orbits off-transit). We will
search for any egress signature, and we will evaluate the COS
capability to measure exoplanet transit signatures in OI 1304 Ang
against the geocoronal 1304 Ang background that varies along the HST
orbit.
GEB is funded by StScI thru HST-GO-11673-01.A

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