J/A+A/587/A57 HR 8799e and HR 8799d spectra (Zurlo+, 2016)
First light of the VLT planet finder SPHERE.
III. New spectrophotometry and astrometry of the HR 8799 exoplanetary system.
Zurlo A., Vigan A., Galicher R., Maire A.-L., Mesa D., Gratton R.,
Chauvin G., Kasper M., Moutou C., Bonnefoy M., Desidera S., Abe L.,
Apai D., Baruffolo A., Baudoz P., Baudrand J., Beuzit J.-L., Blancard P.,
Boccaletti A., Cantalloube F., Carle M., Cascone E., Charton J.,
Claudi R.U., Costille A., de Caprio V., Dohlen K., Dominik C., Fantinel D.,
Feautrier P., Feldt M., Fusco T., Gigan P., Girard J.H., Gisler D.,
Gluck L., Gry C., Henning T., Hugot E., Janson M., Jaquet M.,
Lagrange A.-M., Langlois M., Llored M., Madec F., Magnard Y., Martinez P.,
Maurel D., Mawet D., Meyer M.R., Milli J., Moeller-Nilsson O., Mouillet D.,
Origne A., Pavlov A., Petit C., Puget P., Quanz S.P., Rabou P., Ramos J.,
Rousset G., Roux A., Salasnich B., Salter G., Sauvage J.-F., Schmid H.M.,
Soenke C., Stadler E., Suarez M., Turatto M., Udry S., Vakili F.,
Wahhaj Z., Wildi F., Antichi J.
<Astron. Astrophys. 587, A57 (2016)>
=2016A&A...587A..57Z 2016A&A...587A..57Z (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Planets ; Spectroscopy
Keywords: techniques: image processing - astrometry -
techniques: high angular resolution - techniques: spectroscopic -
methods: data analysis
Abstract:
The planetary system discovered around the young A-type HR 8799
provides a unique laboratory to: a) test planet formation theories; b)
probe the diversity of system architectures at these separations, and
c) perform comparative (exo)planetology.
We present and exploit new near-infrared images and integral-field
spectra of the four gas giants surrounding HR 8799 obtained with
SPHERE, the new planet finder instrument at the Very Large Telescope,
during the commissioning and science verification phase of the
instrument (July-December 2014). With these new data, we contribute
to completing the spectral energy distribution (SED) of these bodies
in the 1.0-2.5um range. We also provide new astrometric data, in
particular for planet e, to further constrain the orbits.
We used the infrared dual-band imager and spectrograph (IRDIS)
subsystem to obtain pupil-stabilized, dual-band H2H3 (1.593um,
1.667um), K1K2 (2.110um, 2.251um), and broadband J (1.245um) images of
the four planets. IRDIS was operated in parallel with the integral
field spectrograph (IFS) of SPHERE to collect low-resolution (R∼30),
near-infrared (0.94-1.64um) spectra of the two innermost planets
HR 8799 d and e. The data were reduced with dedicated algorithms,
such as the Karhunen-Loeve image projection (KLIP), to reveal the
planets. We used the so-called negative planets injection technique to
extract their photometry, spectra, and measure their positions. We
illustrate the astrometric performance of SPHERE through sample
orbital fits compatible with SPHERE and literature data.
Description:
The files contain the wavelength in micrometers in the first column,
the flux in W/m2/mum in the second column and the corresponding error
in the third. We refer to the text for more
informations /Users/alice/paper_hr8799/readme.txt.
Any further question can be addressed to
Objects:
-----------------------------------------------
RA (2000) DE Designation(s)
-----------------------------------------------
23 07 28.72 +21 08 03.3 HR 8799 = HD 218396
-----------------------------------------------
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
sp8799d.dat 39 39 HR 8799d spectrum
sp8799e.dat 39 39 HR 8799e spectrum
--------------------------------------------------------------------------------
See also:
J/ApJ/761/57 : CHARA array angular diameters of HR 8799 (Baines+, 2012)
Byte-by-byte Description of file: sp8799d.dat sp8799e.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
6- 13 F8.6 um lambda Wavelength
15- 26 E12.6 W/m2/um Flux Flux
29- 39 E11.6 W/m2/um e_Flux rms uncertainty on Flux
--------------------------------------------------------------------------------
Acknowledgements:
Alice Zurlo, alice.zurlo(at)mail.udp.cl
References:
Zurlo et al., Paper I 2014A&A...572A..85Z 2014A&A...572A..85Z
Mesa et al., Paper II 2015A&A...576A.121M 2015A&A...576A.121M
(End) Patricia Vannier [CDS] 10-Nov-2015