spectro-aras.com

Hi all,

The french association "OATBL" (aka les Observateurs Associés du Telescope Bernard Lyot") is composed of volunteers accepting to spend a week as "Observateur de service" with the operators of the 2 meters Bernard Lyot Telescope at Pic du Midi de Bigorre.

If some conditions are met (Scientific interest, planning completed,...), the OATBL member on duty has the possibility to submit one observation request (1 hour for a full week mission, 30' for a short mission) . If the observation is accepted, processed results are delivered within few days.
As the OATBL observer don't always has a subject of observation, he can carry an aim proposed by the amateur spectrography community (Thru the OATBL bureau).

Recently we had two observations accepted (within a large period of anticyclonic high pressure).
- the first was proposed by the M.Verlinden/JP.Godard team at the T60 (60cm Newton at Pic du Midi) : Supernova 2016gxp http://www.spectro-aras.com/forum/viewt ... f=6&t=1593
- the second was proposed by Oliver Garde as a spectro polarimetry calibration exemple : "Beta CRB"

Should you need a high resolution spectrum (still not available in Polarbase), don't hesitate to send a 15 lines observation request to the OATBL bureau... It could work...
(Note: The allocation scheme of this discretionnary observation time clearly does not allow a survey of a particular star.).

The OATBL President

On 12/12/2016 OATBL Observer Merry Anfray agreed to request BL CAM sprectrum(HR) on his discretionnary observation time as suggested by S FAUVAUD.
Data has been delivered after successul observation.

Reasons for observation are presented here:

"Etoile de population II, BL Cam est particulièrement déficiente en métaux ([Fe/H] = –2.4 dex). Les caractéristiques physiques de l’étoile actuellement disponibles reposent toutefois seulement sur des méthodes photométriques (McNamara & Feltz 1978, PASP 90, 275). Les données spectroscopiques font en effet défaut. L’objectif est donc de réaliser un spectre de BL Cam pour en déduire précisément ses paramètres physiques (Teff, log g, abondance des éléments présents dans l’atmosphère…).

Compte tenu de la faible luminosité de l’étoile, un temps d’acquisition de 56 minutes est souhaité pour le spectre. Une telle durée, qui correspond à celle d’un cycle de pulsation de l’étoile (0,0391 jour), devrait permettre, d’une part, de moyenner les variations et l’évolution (si elles existent) des raies spectrales au cours de la pulsation, et, d’autre part, d’augmenter le rapport signal sur bruit du spectre. "

OATBL Bureau