ID Code_agency lname email title instrument other_instr nights Moon lst_opt lst_early lst_late nights AgencyRank Ranking ScheduledDate NightsSch FirstHalf ID Note SA qtype giq unacceptable joint joint_nights accepted_id dbo_justification_2003B.prop_id unaccept targets F8 France Catala Claude.Catala@obspm.fr Imagerie AOB des champs des cibles de la mission spatiale COROT AOB IR 1.5 14 02:00 00:00 12:00 1.5 5 0.27 9/28/2004 1.5 Y Not Applicable Not Applicable une demi-nuit pour nos cibles autour de 7h, en milieu ou en fin de semestre, et 2 demi-nuits pour les cibles autour de 19h, en d\'ebut de semestre. NO 0 COROT est une mission spatiale du CNES, pour l'\'etude des int\'erieurs stellaires par ast\'erosismologie et la recherche d'exoplan\`etes par d\'etection de transits plan\'etaires. Pour pr\'eparer la s\'election des \'etoiles-cibles de la partie ast\'e F15 France Galland Franck.Galland@obs.ujf-grenoble.fr Investigating low-mass companions around early type stars AOB IR 6 7 07:00 02:00 12:00 4 8 0.43 1/23/2005 4 Y Not Applicable Not Applicable YES 25 We have started an AO systematic search for low mass companions (BDs) around A-F type stars, in complement with a radial velocity survey. This allows for the first time to extend the planet/BD systematic search around stars earlier than F8 and hence to ex F16 France LEMAIRE jean-louis.lemaire@obspm.fr The spatially resolved dynamics of star-forming regions, using PUEO+GriF AOB GRiF 5 14 06:00 04:00 08:00 3 13 0.70 1/27/2005 3 Y Not Applicable Not Applicable NO 5 Our objective is to investigate early stages of star formation in OMC1, building on earlier work  with AOB-GriF which (i) allows observation of shocks in unprecedented detail (ii) shows that  H$_2$ emission in OMC1 is partly due to the presence of early p F39 France Veillet veillet@cfht.hawaii.edu Binarity in the Solar System AOB IR 6 11 Any Any Any 2 15 0.81 1/26/2005 3 Y Not Applicable Not Applicable The Milky Way should be avoided... NO 0 This proposal aims to a study of the binarity in the Solar System. A binary object is a pair of objects of similar size, instead of the more studied asteroid-moon systems where faint companions of big asteroids are generally looked for. With the discov F22 France Forveille Thierry.Forveille@cfht.hawaii.edu Stellar multiplicity and extra-solar planet formation AOB IR 2 14 Any Any Any 0 17 0.92 9/26/2004 2 Y Not Applicable Not Applicable NO 0 Two main scenarios are competing to explain planet formation: gas accretion onto a solid core, versus disk instability possibly enhanced by a close stellar/substellar companion. We propose a systematic, statistically significant, adaptive optics sea F35 France Chauvin gchauvin@eso.org Stellar and Substellar Multiplicity of F7-K Stars at Long Periods AOB IR With KIR 5 14 03:00 02:00 04:00 3 18 0.97 3 Y Not Applicable Not Applicable NO 0 We propose, for the period 2004B, to start a deep imaging survey with PUEO/KIR, at CFHT, to determine the multiplicity of F7-K dwarfs \textbf{at long periods ($\rm{P}=[10,10\,000]~\rm{yrs}$) within the stellar and substellar regime}. This key program, whi F30 France Israel gianluca@mporzio.astro.it PROBING THE AXPs-SGRs LINK WITH CFHT ADAPTIVE OPTICS AOB IR 3 11 21:00 20:00 22:00 1.5 20 1.08 Not Applicable Not Applicable First half of August is preferred NO 0 This proposal addresses the issue of the IR (variable) emission of two classes of peculiar objects, Anomalous X--ray Pulsars (AXPs) and Soft Gamma--ray Repeaters (SGRs), thought to be linked at same level. Currently, the AXP and SGR IR-to-X--ray emission 10.5 C23 Canada Roberts roberts@physics.mcgill.ca Optical Counterparts to X-ray Pulsars and Neutron Star Candidates AOB IR 1 10 20:00 19:00 21:00 1 22 1.26 Not Applicable Not Applicable NO 0 Optical observations can be used to identify radio quiet neutron stars and to constrain models of high energy pulsed emission. We propose to use the PUEO/KIR to search for optical counterparts of 5 X-ray sources in the Galactic plane which are neutro H25A Hawaii Stalder stalder@ifa.hawaii.edu AO Studies of Radio Sources Near Bright Natural Guide Sars AOB IR 23:00 3.00 12 0.77 9/26/2004 3 Y H53A Hawaii Ftaclas ftaclas@ifa.hawaii.edu Adaptive Optics Search for Substellar Companions Around White Dwarfs AOB IR 0:00 1.00 9 0.58 38255.00 1 Y 4.00 14.50 C2 Canada Willott chris.willott@nrc-cnrc.gc.ca The quasar luminosity function at z=6 from the CFHTLS CFHTIR 2 14 05:00 03:00 07:00 2 13 0.74 11/22/2004 2 Y Not Applicable Not Applicable Availability of W1 and W2 fields. NO 0 We are using the CFHT Legacy Survey Wide component to compile the largest sample of redshift $z\sim 6$ quasars. Making conservative assumptions, we expect to find 40 quasars (twice as many as in the SDSS).  Our $z'$-band flux limit is a factor of 10 lo 2 F4 France Bouvier jbouvier@obs.ujf-grenoble.fr Proper motion of brown dwarf candidates in the Hyades cluster : a near-IR follow-up CFHTIR 3 14 04:00 03:00 05:00 3 1 0.05 11/24/2004 3 Y Not Applicable Not Applicable NO 0 The deep, wide-field (I,z) survey we performed on the Hyades cluster using CFHT 12K revealed 105 low-mass cluster candidates (M$\leq$0.25M$_\odot$), including 68 brown dwarf candidates (M$\leq$0.075M$_\odot$). We propose here to get K-band images for t F40 France Moraux Estelle.Moraux@obs.ujf-grenoble.fr Near-infrared follow-up of Pleiades and Blanco~1 brown dwarf candidates CFHTIR 3 14 03:00 02:00 04:00 3 12 0.65 11/27/2004 3 Y Not Applicable Not Applicable NO 0 From deep wide-field $I$, $z$ surveys performed in the Pleiades and Blanco~1 young open clusters in Dec. 2000, we have identified very low mass star and brown dwarf (BD) candidates and we derived the mass function (MF) for both clusters down to 0.03 $M O3 Opticon Giovanardi giova@arcetri.astro.it NIR SCALING RELATIONS AND EVOLUTIONARY STATE OF M81 GROUP DWARF GALAXIES CFHTIR 3 12 09:00 08:00 10:00 3 25 1.35 Not Applicable Not Applicable NO 0 Dwarf galaxies are recognized as a cornerstone in our understanding of the physical processes that govern galaxy formation and evolution. However, massive optical surveys such as the SDSS fail to place significant constraints on the dwarf population 6 K6 Korea Kim dckim@astro.snu.ac.kr CFHT-IR K$'$-band Imaging Observations of Ultraluminous Infrared Galaxies and Field QSOs. CFHTIR 2 10 05:00 00:00 10:00 2 1 0.15 11/30/2004 2 Y Not Applicable Not Applicable Early 2nd or 3rd week of Dec., 2004 (Best), January, 2005 (better), other (acceptable) NO 0 To study evolutionary connection between ULIGs and QSOs, we propose CFHT-IR K'-band imaging observations for these objects. To properly trace the evolutionary connection, sample selection is crucial in this study. For the ULIG sample, we have selected a 2 T5 Taiwan Lim jlim@asiaa.sinica.edu.tw Optical/Near-IR and HI Imaging of QSO Host Galaxies CFHTIR 1 14 Any Any Any 1 10/22/2004 1 Y Not Applicable 0.65'' < IQ < 0.80'' Avoid times when program objects within 45 degrees of Moon NO 0 We are conducting an ongoing program to image low-redshift QSO host galaxies in neutral atomic hydrogen (HI) gas with the Very Large Array. Our results show that many of these galaxies exhibit HI tidal features that can be traced to interactions with a n 1 11 C10 Canada Carney bruce@physics.unc.edu Line broadening in luminous metal-poor stars: Turbulence or Absorption of Planets? Gecko Red + Cafe 3 14 N/A N/A N/A 3 5 0.29 12/21/2004 3 Y Not Applicable Not Applicable Please avoid November 4-12 (Gemini Board of Directors) NO 0 In a study of 134 field stars and a comparable number of red giants in the globular cluster M3, we find that about half of the most luminous red giants and about half of their red horizontal branch star descendents rotate at significant rates ($\appro C5 Canada Manset manset@cfht.hawaii.edu Spectroscopy of hot star candidates with recently formed circumstellar dust Gecko Red + Cafe 4 11 07:00 04:00 10:00 4 12 0.69 12/23/2004 4 Y Not Applicable Not Applicable From our February 2004 observations, we have found out that a Full Moon makes acquisition and observation of the faint targets difficult. We would prefer to be scheduled a few days away from the Full Moon if possible. NO 0 The aim of the program is to determine the physical parameters of newly found optical counterparts of IRAS sources with infrared colors indicative of warm circumstellar dust which seem to belong to a {\bf new distinct group of dust-forming hot stars C1 Canada Landstreet jlandstr@uwo.ca Magnetic measurements of very slowly rotating magnetic Ap stars Gecko Red + Cafe 2 14 01:00 Any Any 2 14 0.80 12/29/2004 2 Y Not Applicable Not Applicable NO 0 A small fraction of the magnetic Ap stars rotate extremely slowly, with periods of several years to several decades. With the currently known sample of 22 stars (mostly found by us), it is feasible to investigate the physical processes that have slowe C3 Canada Rice rice@brandonu.ca Doppler Imaging of the Young Active SLowly Rotating Star PW And Gecko Red + Cafe 4 14 00:00 22:00 02:00 4 17 0.97 8/25/2004 4 Y Not Applicable Not Applicable It is absolutely essential that we have 2 nights on the telescope, then 2 off, then 2 on again in order to have the excellent phase coverage required for the star. NO 0 Previous Doppler Images of the very young main-sequence active stars LQ~Hya (K2V) and EK~Dra (G1.5V) have shown that the predominant location of activity on LQ Hya is more equatorial and that of EK Dra is primarily polar. This runs counter to the expected C25 Canada Bohlender david.bohlender@nrc-cnrc.gc.ca A large-scale investigation of the small-scale structure of the interstellar medium Gecko Red + Cafe 2 14 00:00 00:00 04:00 2 19 1.09 8/31/2004 2 Y Not Applicable Not Applicable I am unable to observe in 2004 August.  Time late in the semester is not particularly useful since winter targets have been observed in a previous run. NO 0 A quick search of the CFHT archive reveals that there are high signal-to-noise, high-resolution ($R = 120,000$) spectra of the Na I D lines for well over 100 objects, many of which are early-type stars.  These observations date back to at least 1997, and 15 F23 France ROUEFF Evelyne.Roueff@obspm.fr The ionization rate of hydrogen in the neutral interstellar medium Gecko Red + Cafe 4 14 00:00 22:00 04:00 2 11 0.59 7/26/2004 2 Y Not Applicable Not Applicable We would prefer to be able to observe $\zeta$ Per during the largest amount of hours. NO 0 Sensitive searches will be made for interstellar absorption lines of the reactive ions H$_2$O$^+$ and OH$^+$ in directions where interstellar H$_3^+$ has been previously observed. These ions offer the most direct tracers of the ionization of H$_2$ an O1 Opticon Israelian gil@ll.iac.es Have the parent stars of extra-solar planetary systems engulfed planets? Gecko Red + Cafe 4 1 Any Any Any 2 14 0.76 12/31/2004 2 Y Not Applicable Not Applicable We need October-December period to observe our targets NO 0 More than 100 planetary systems have been discovered to date. High quality spectroscopic observations with a VLT/UVES have revealed a significant content of the very fragil $^6$Li isotope in the atmosphere of one of the planet host stars (Israelian e F31 France Vidal-Madjar alfred@iap.fr The evaporating planet HD\,209458b : Search for additional escape signatures. Gecko UV + Cafe 2 14 22:00 21:00 22:00 2 3 0.16 8/1/2004 2 Y Not Applicable Not Applicable Scheduling is critical (transits); see Section 13 for more details. NO 0 Using HST, we detected an extended upper atmosphere in the extra-solar planet HD\,209458b (Vidal-Madjar et al., 2003, Nature 422, 143). The observations reveal an absorption of 15$\pm$4\% of the stellar Lyman-$\alpha$ emission line during the planetary 6 K3 Korea Galazutdinov gala@boao.re.kr Linear, carbon-bearing, interstellar molecules. Gecko UV + Cafe Gecko BLUE + Cafe 3 14 00:00 Any Any 2 6 0.92 12/27/2004 2 Y Not Applicable Not Applicable First half of September is a best period for our proposal. NO 0 We propose to continue the search for fine structures inside the profiles of weak diffuse interstellar bands (DIBs) in the spectra of bright, reddened stars. Our recent results clearly demonstrate that the high resolution is crucial: such substructures ha K10 Korea Lee hwlee@sejong.ac.kr Deep Raman Spectroscopy of Symbiotic Stars Gecko Red + Cafe ESPADONS (nonpolarimetric mode) 1 14 N/A N/A N/A 1 3 0.46 1/29/2005 1 Y Not Applicable Not Applicable Our prime target is V1016 Cyg, which can be best observed before October. NO 0 We propose long exposure spectroscopic observations of several symbiotic stars exhibiting Raman scattered O~VI~6825, 7088 features. With deep exposure data, we expect to secure the broad feature at 4975 \AA\ that is proposed to be formed via Raman sc 3 24 C14 Canada Dennis Dennis.Crabtree@nrc-cnrc.gc.ca Images for Canadian Amateur Astronomer Contest MegaPrime 1 10 N/A N/A N/A 1 1 0.06 Regular IQ > 1.2'' Target to be selected early in the semester. NO 0 Canadian amateur astronomers will compete for one hour of Canadian time on CFHT to obtain images which will be used to promote Canadian astronomy and may also be used for scientific purposes. C17 Canada Allen lallen@astro.ubc.ca Determining the Kuiper belt Size Distribution MegaPrime 9.2 4 02:00 00:00 Any 9.2 2 0.11 Regular 0.65'' < IQ < 0.80'' The months of August and December are undesireable for this project, as in August the ecliptic is too low and in December the observable fields are in the galactic plane. NO 0 We propose to conduct a deep pencil-beam survey of the Kuiper belt over one square degree to $g'=27.2$. Recent observations with the HST/ACS have shown that the luminosity function of Kuiper belt Objects is best fit with a double power law, however the sh C24 Canada Allen lallen@astro.ubc.ca The Sub-Kilometer Main Belt Asteroid Population MegaPrime 7.8 4 Any Any Any 7.8 3 0.17 Regular 0.80'' < IQ < 1.0'' Details of scheduling will depend on when/if the SIRTF observations are scheduled. NO 0 We propose a series of observations to coordinate with Spitzer discoveries of sub-kilometer (and larger) asteroids over $\approx4$ square degrees, in order to determine the size and albedo distribution of these small main belt asteroids. These ground-ba C7 Canada Hoekstra hoekstra@cita.utoronto.ca Comparison of the weak lensing mass to the baryonic constituents in X-ray luminous clusters of galaxies MegaPrime 38.2 8 Any Any Any 38.2 4 0.23 Regular 0.65'' < IQ < 0.80'' NO 0 We propose to observe 19 X-ray luminous galaxy clusters in order to determine their masses via weak gravitational lensing.  This effort is part of a broader systematic programme to study the relationship between baryonic tracers of cluster mass and the ac C21 Canada Bickerton bick@physics.mcmaster.ca Darkness on the Edge of Town:  Probing the size distribution of Kuiper belt down to 200 meters MegaPrime 6 9 18:00 15:00 21:00 0 6 0.34 Regular IQ > 1.2'' NO 0 Using MEGACAM as an high speed multi-object photometer we will monitor a patch of bright stars for occultation by solar system objects.   Our observations will be tuned to detect $\sim 200 m$ sized bodies in the Kuiper belt.   This innovative use of the w C6 Canada Gilbank gilbank@astro.utoronto.ca Tracing Galaxy Transformation around a pair of z=0.4 Clusters with Megacam MegaPrime 11.7 7 03:00 01:00 05:00 11.7 7 0.40 Regular 0.55'' < IQ < 0.65'' NO 0 We propose to use the unique wide-field capability of Megacam to study galaxy transformation in the supercluster environment around a pair of galaxy clusters at z=0.41. We will use our extensive spectroscopic survey undertaken on 8-m class telescopes to c C16 Canada Courteau courteau@astro.queensu.ca The Halo Shape, Metallicity, and Substructure of Three Nearby, Massive Galaxies MegaPrime 16.5 5 05:00 20:00 13:00 5.5 8 0.46 Regular 0.55'' < IQ < 0.65'' \vspace{-0.48cm}\hspace{4.cm} Low airmass, 6 day moon is the limit for the $r^\prime$ observations. The $i^\prime$ observations can be taken at low airmass, in grey/bright time, if $i^\prime$ sky brightness is indeed independent of moon phase as documente NO 0 We propose to resolve the stellar populations of the halos of three nearby, massive disk galaxies (NGC\,253, NGC\,2403, M81/M82) using deep images with MegaCam. These data will provide star counts and colour-magnitude diagrams 1-2 magnitudes below t C8 Canada Kavelaars jjk@hia.nrc.ca The irregular satellites of Uranus: the era of impact MegaPrime 18 7 21:00 20:00 22:00 18 9 0.51 Regular 0.80'' < IQ < 1.0'' Target can be observed when at elongations larger than 160 degrees. NO 0 We will use the CFHT MEGACAM to conduct a pencil beam survey searching for small irregular satellites of Uranus.   Our goal is to probe the small size distribution of the irregulars nearest to Uranus in a search for evidence of size and orbit segregation C20 Canada Kalirai jkalirai@physics.ubc.ca The White Dwarf Initial-Final Mass Relationship MegaPrime 4.4 7 21:00 17:00 01:00 4.4 11 0.63 Regular 0.80'' < IQ < 1.0'' Fields above did not work: IQ=0.8-1, 4.4 hours, LST=19:00:00 (NGC6705) and 23:30:00 (NGC 7654) +/-3hours, $\pm$7days from newmoon. NO 0 We propose to obtain very deep photometry for two rich open star clusters, NGC 6705 (M11) and NGC 7654 (M52).  Given the young ages ($<$few hundred Myrs) and relatively small distance moduli ($<$12.5), high S$/$N g$'$,r$'$ = 25 photometry of a large area C19 Canada Crotts arlin@astro.columbia.edu Microlensing in M31 at Large Distances and for Large Masses MegaPrime 8 14 01:00 18:00 08:00 8 SNAP #VALUE! Snapshot IQ > 1.2'' Observations are much more effective if scattered throughout entire semester, Aug - Jan. Also c.f.~\S 15. NO 0 We have recently completed a survey of microlensing in M31 that has discovered several events on $\sim 10^6$s timescales, corresponding to about $0.5~M_\odot$ or slightly less. A large number of events of this nature are also being found by the wider C4 Canada Innanen kiminn@yorku.ca Search for L$_{5}$ Venus Trojans MegaPrime 3.5 10 Special Special Special 3.5 18 1.03 Regular 1.0'' < IQ < 1.2'' One hour before dawn in December (around Venus L$_{5}$ maximal elongation) YES 7 The presence of Trojan-type asteroids in the Solar System has a distinguished history, now well exceeding a 2-century timeline. The first such object has been discovered at Jupiter's L$_{4}$ site in 1906. Since then, a large number of Jupiter Trojans hav C9 Canada Barkhouse wbark@head-cfa.harvard.edu Quantifying Environmental Effects on the Cluster Dwarf Galaxy Population MegaPrime 20.2 6 Any Any Any 20.2 SNAP Snapshot IQ > 1.2'' None NO 0 Studies of galaxy cluster luminosity functions (LFs) have provided evidence for significant variations in the shape of the LF. These changes are shown to correlate with cluster environment and are more pronounced for the dwarf galaxy population, repr C11 Canada Lee hlee@astro.umn.edu Searching for Populations of Dwarf Galaxies in X-Ray Luminous and X-Ray Faint Groups of Galaxies MegaPrime 23 3 Special Special Special 23 20 1.14 Regular 1.0'' < IQ < 1.2'' NO 0 Poor groups of galaxies are the most common environments for galaxies in the nearby Universe. Most studies of poor groups have been limited either to our Local Group or to much richer, X-ray luminous systems. It remains yet unclear whether (1) the Loc C12 Canada Gladders gladders@ociw.edu Galaxy Clusters as a Dark Energy Probe MegaPrime 45.5 9 Any Any Any 45.5 21 1.20 Regular 0.55'' < IQ < 0.65'' YES 84.5 Understanding dark energy, the most dominant and least understood component of the universe, is the single greatest goal in cosmology (and arguably, all of physics) for the next decade. The quest to understand dark energy keys on attempts to measure 15.9666667