Teleconferences 11/14/00 Shorthand notes by Gerson. Very brief - just to jog your memory. * Discussion of work in progress: Reynald: Paris activities Software for HiZ Pierre Search software Analysis. rate paper CFHT search Ravel only was found plus spectrum ________________ Ariel: group working on: Low redshift spectroscopy SN Calculator ________________ Brad Schaefer: observed 30 SNe with Qwest Hopes to get 50 SNe around z~0.2 at McDonald & Kitt Peak ________________ CalTech Spectroscopic ID of galaxies MARK (working with Ellis) _________________ * SN Factory activities Haleakala 1.2m 4Kx4K Palomar 1.2m Schmidt 28K x 16K ________________ Wood -Vasy automatic subtractions ________________ Greg: SNIFS 6" x 6" field 0.4" pixels under construction in Lyon 2 spectrographs + guider _______________ Saul: Univ. Hawaii 2.2 m telescope Mauna Kea Telescope contract 20% for 3 years 10% for 4th year Start 2002 Expect 300 type Ia SNe out of Hubble flow ________________ ________________ * Don: Report on LBL CCD's Butler - Marcy group LBL's 2Kx2K in use, obtain better psf ARJUN Dey:at KPNO Red Response is better than LORAL CCD's CCD's act like "Emulsions" we see mu's & e's: low energy e's called "spots," more energetic e's called 'worms' Low level site studies * 180m underground Oroville. No CR's but see worms. In additional vault - radiation much reduced. * Berkeley Low Counting Facility: find CR but few worms or spots Find Pb shielding, (1/4"Pb) lowers radiation by factor > 3 200mu depleted CCD's better psf than 300mu, yields 1/2 as wide PSF with 200µ; clean tracks, however QE falls off, lowered by 100-150 Å Steve: succeeded in reducing amplifier noise from 4e -> 2e by transistor geometry improvements Keck: Will ESI with LBL chip be ready for our run? ___________________ ___________________ * Desired time assignments: Keck 6 nights 1, LRIS 5, ESI (obtained) March - April nights assured March - April schedule: 25-29 March - Ref's at CTIO 15-19 April - search at CTIO, search at CFHT 15-17 April 20-25 April Keck Perhaps we can obtain some of Ellis' Keck time after that Reynald should get the CFHT dates ____________________ We have - put in proposal for follow up work at Gemini & VLT Spectroscopy & IR possible ISOBEL is looking into UK time & US time? Who does scheduling? VLT Chris is checking on it ISAC for May 6 z = 1 should be taken at Max, z = 0.5, week after Max ____________________ Peter - For z = 0.8, IR Measurement at second peak will take all night if z ~ 1 measure as close to max as possible _____________________ * Plans for HST, Peter 5 SNe for HST 3 @ z = 0.8, and 2 @ z = >1 For each SN: 5 ltcv points for 2 orbit, at first for 2 epochs 3 orbits, for last 3 epochs move to low CTE region @ pixel x = 200, y = 200 at first give: 10 targets in 1º radius, reduce to 5 after 1 week Example of scheduling: Wed Co-ordinates to HST, Mon start observation VLT spectroscopy as back up _____________________ _____________________ * Saul: Suggested telescope time order - each symbol represents one night for search and spectroscopy as indicated: CFHT CFHT CFHT CTIO CTIO CTIO LRIS ESI ESI HST request must go in ESI CTIO confirmation of CFHT SNe possible _____________________ * Reynald: Discussion of previous CFHT runs Why did we not find z >1 SNe last time? 2 first runs in 1999, 2 pointing of 3 hours. I-Filter Spring 2000 2 1/2 hours in I-Filter Found Ravel, z = .86 light curves Max at 24.5 Mag (looks wrong) Was there light on reference? What about other SNe? Post Mortem is needed, detection efficiency? Can there be voids @ (z = 1), which we happened to hit? Unlikely, S/N ~5 ___________________ * Rob: Future Plans Compare 2 fields one night appart to look for fakes Take some overlap between 2 telescopes Try for 7 sigma S/N, Confirmation of SNe at KPNO important ____________________ Greg: 2000A run CFHT follow up Berlios has only 1 emission line @ 6980A°, Resolution 25A° this allows 2 possible candidate redshifts. Also HST flux measurements were flat. Conclusion: NOT SN Looked off center at first but is actually on core Result: ~3 AGN + 1 type Ia SN. __________________ Check on: Cross telescope subtraction? I bands are different. Are there some common fields already? Reynald: Compared Astrometry . Offsets are the same. Good to 0.1" Rob: Some offsets are the same, but some are up to 0.4" different, Redo finding charts? __________________ __________________ * General remarks interspersed with Plans and post mortems Pilar: Are the rates dropping at z >1 Peter: Rates increase above z=1 Uses empirical rates from the Hi z team results _________________ Sebastien: what are the Keck search details for Albinoni MI = 24.7 was near to cutoff Keck I filter wider but also more sky? Z filter?? Is it advantageous? sky brighter, but CCD dying ISOBEL Previous run @ CFHT Run 99b one SN was found: Ravel however bad weather off & on 1 object z = .94 gal, no SN visible __________________ Reynald: Most recent run with R & I ref images Fringes in I bad 10 pointings 2x 12 mins in R & I 8 pointings 2x 8 min in R & I use to check color test? (Ariel) Candidates S/N > 7 High S/N in R, Not in I if Not in R, but Yes in I could be high z object ________________________ Rob: Take zero points for photometric Ref Run Try to get magnitude on diff stars, Calibrate ref runs _______________________ Gerson 20% overlap between fields at the 2 Telescopes is desirable _______________________ cross check by Reynald - Rob _______________________ Rob Calibrate on a 2 m telescope on fields we plan to use, perhaps fields we already looked at _______________________ Prob of hitting a void or overdensity, NOT likely. Void size ~ 0.02 in delta z. _____________ 1/2 data of night should be subtracted from each other _____________ Reynald will do statistical analysis _____________ Paralactic angles? -45° to +45° Equatorial field - stick to one position angle? or use 2 position angles? Peter: Riess quotes; - John Tonrey observed highest red shift Sne, two diff angles worked for him. _________________ Ariel's examples worse than our observation. Will try with Albinoni Look at Berlioz 0.7" to 1.0" slit width Greg typed the Pivot star Ariel: Will study past spectra for pivot star color, slit size etc. Will co-ordinate with Greg _________________ Look at Hi z team observations says Peter ________________ Try to Find data overlap at CTIO and CFHT for comparison. Are colors useful? if we have no other info. Ariel has notes on our previous attempts. If perfect nights at both telescopes, can we do cross telescope subtractions in diff colors? __________________ Choosing fields: Greg will choose fields. Rob will choose Standard stars in Feb ____________________ * Photometric Red shifts are they useful? Rob No Ariel Yes ____________________ Photometric Red shifts worked at HST but they had UVRI.... 9 filters Subaru could get us photometric Red Shifts? Ariel will ask. ____________________ * Tools we need ESI tools Generate a set of images from Ref images to check for problems ____________________ give RA & DEC on each image, & on files get RA, DEC x, y for 1950 & 2000 co-ords. ____________________ Reylight program needs to be updated ____________________ End