In the same section :
AMBEROK official document
Contrat post-doctoral ouvert sur des observations VLTI/AMBER
List of Hotels in Grenoble
Postdoctoral and Ph.D. positions in Infrared Interferometry at MPIFR (Bonn)
Presentation and video clips of the AMBER workshop 2007 (previously "Program")
Opening for a post-doctoral position on VLTI/AMBER observations
AMBER Scientific Workshop (Grenoble, 7-8 Mar 2007)
First publication : 3 March 2007, publicated:
27 August 2007, by
Rationale: AMBER/VLTI has now been offered since October 2005 to the ESO community. We would like to gather the astronomers who have obtained AMBER data in order to publicize the various results and share our common experience on the instrument. This will also be the opportunity to give some information on the current status of the instrument. This workshop will last 1.5 day and will be followed by the meeting of the AMBER science group.
Organizer: F. Malbet, AMBER Project Scientist, together with the AMBER science group (SGR)
Venue: Laboratoire d’Astrophysique de Grenoble (Grenoble, France) from Wednesday 7 March 2007 at 9:00am to Thursday 8 March 2007 at 14:00pm.
Hotels: see the list of hotels. There is also the Hôtel Ibis Université which is located on Campus on the A/C tram line which might be an interesting solution a little bit ex-centered compared to Grenoble downtown but certainly more quiet.
Food: see the restaurants and bars section on the IAUS243 web site.
We have limited resources to help young researchers to participate to this workshop. Please send an email to F. Malbet.
before Friday 2 March 2007.
We plan to have a buffet for Wednesday and Thursday lunches.
Program: see the final program
List of participants: total of 40 participants
B. Acke (KUL, Leuven, Belgium)
E. Altariba (LAOG, Grenoble, France)
S. Antoniucci (OAR, Roma, Italy)
M. Benisty (LAOG, Grenoble, France)
J.-P. Berger (LAOG, Grenoble, France)
A. Chalabaev (LAOG, Grenoble, France)
A. Chelli (LAOG, Grenoble, France)
O. Chesneau (OCA/Gemini, Nice, France)
F. Cusano (TLS, Tautenburg, Germany)
D. Defrère (IAGL, Liège, Belgium)
B.-O. Demory (Obs. Genève, Switzerland)
M. Desmet (KUL, Leuven, Belgium)
E. Di Folco (Obs. Genève, Switzerland)
T. Driebe (MPIfR, Bonn, Germany)
G. Duchêne (LAOG, Grenoble, France)
A. Dutrey (L3B, Bordeaux, France)
G. Duvert (LAOG, Grenoble, France)
T. Forveille (LAOG, Grenoble, France)
R. Foy (CRAL, Lyon ,France)
D. Fraix-Burnet (LAOG, Grenoble, France)
A. Isella (OAA, Firenze, Italy)
O. Hernandez (LAOG, Grenoble, France)
G. Li Causi (OAR, Roma, Italy)
F. Malbet (LAOG, Grenoble, France)
F. Millour (MPIfR, Bonn, Germany)
A. Meilland (OCA/Gemini, Nice, France)
J.-L. Monin (LAOG, Grenoble, France)
J. Olofsson (LAOG, Grenoble, France)
I. Percheron (ESO, Garching, Germany)
R. Petrov (LUAN, Nice, France)
P.-O. Petrucci (LAOG, Grenoble, France)
J.U. Pott (UoC, Köln, Germany)
A. Richichi (ESO, Garching, Germany)
K. Shabun (ESO, Garching, Germany)
M. Swain (JPL, Pasadena, USA)
E. Tatulli (OAA, Firenze, Italy)
M. Vannier (UC/ESO, Santiago, Chile))
T. Verhoelst (KUL, Leuven, Belgium)
G. Weigelt (MPIfR, Bonn, Germany)
W.-J. de Wit (Univ. OF Leeds, UK)
G. Zins (LAOG, Grenoble, France)
Contributions: all scientific contributions are welcome (oral talks or posters). Please send an email to F. Malbet.
before Friday 2 March 2007.
B. Acke (Leuven, Belgium): AMBER observations of a binary Post-AGB star (with P. Deroo and T. Verhoelst)
F. Cusano (Tautenburg, Germany): Pre-main sequence spectroscopic binaries suitable for VLTI observations
O. Chesneau (OCA/Gemini, France): The potential of AMBER to study nova outbursts
G. Duvert (LAOG, Grenoble): Status of AMBER data reduction
A. Isella (OAA, Italy): Observation of the Herbig Ae/Be star HD 104237
O. Hernandez (LAOG, France): Accurate diameter measurement of Betelgeuse using the VLTI/AMBER instrument
G. Li Causi (INAF-Roma, Italy): Observations of faint sources with AMBER and the AMDC software (TBC).
F. Millour (MPIfR, Germany): Differential phase and its application with AMBER
A. Meilland (OCA/Gemini, France): Observations of hot active stars.
I. Percheron (ESO, Germany): AMBER data reduction, the ESO point of view.
R. Petrov (LUAN, France): Status of the VLTI and of AMBER
J.U. Pott (Univ. Cologne, Germany): VLTI observations of objects in the central parsec of the Milky Way
A. Richichi (ESO, Germany): Observations of the Mira star IW Hya
A. Richichi (ESO, Germany): experience on using AMBER with FINITO and information for the next call for proposals
K. Shabun (ESO, Germany): Interferometric investigations of eclipsing binaries as a key to an improved distance scale
E. Tatulli (OAA, Italy): Observations of the CO bands in 51 OPh with AMBER
M. Vannier (UC/ESO, Chile)): High-precision on the differential phase in low-resolution mode
T. Verhoelst (Leuven, Belgium): AMBER simulations of evolved stars with molecular layers
W.J. de Wit (univ. Leeds, UK): AMBER observations of a peculiar post-red supergiant star
G. Zins/E. Altariba (LAOG, Grenoble): interface of the amdlib software with Yorick.
Note on limiting magnitude on FINITO in P80 CfP
13 March 2007, by Jörg-Uwe Pott
Since we discussed at the workshop the limiting magnitude of using FINITO+VLTI in the current ESO-CfP (is the limit H=3 referring to total flux (due to IRIS) or correlated flux (due to FINITO itself)), I posed this question to ESO to clearify the situation.
In the actual CfP is written (p.37, Sect.6.12.3) that for the use of FINITO, the ’limiting correlated magnitude’ is H=3. On the other hand the H=3 limit appear to come from IRIS (to be used in fast mode to use FINITO). That would mean: H=3 is a ’total flux limit’, instead of the given ’correlated flux limit’. This can be important, since the target stars are nearby and typically resolved.
With a total flux limit of H=3 and a minimum visibility of 15% (as given in the actual CfP), you would increase the number of targets.
ESO clearification for the actual period
In principle it is IRIS stopping to go fainter on FINITO but we were only successfully [tracking] fringes [on resolved sources] at 15% on a <1 Hmag source. [...]
Thus the statement of "correlated magnitude" is correct and possible after more standard operation on a much larger sample of targets we will be able to possible create some sort of lookup table for Visibility vs H magnitude as it seems that the constraints are not simply the 2.5*log(Vis) if you really want to be accurate.
So to conclude we offer it with the correlated limiting magnitude of 3 and the minimum V of 15% and most probably for the coming periods we will be able to improve on these numbers but for now these numbers stand.
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