From: Tony Spadafora (ALSpadafora@lbl.gov)
Date: Wed May 29 2002 - 18:57:46 PDT
Attn: Reynald, Pierre, Julian, Sebastian
Below is Rob's plan for the next WIYN night, this Friday May 31. (Thanks
Rob).
At last week's SCP Exec Committee meeting the question arose whether we
should use time to get another lightcurve point for any CFHT candidates.
(We have little CFHT left from our allocated 15 hr/field for when the
12k camera is back on in June, and our luck with Mauna Kea weather has
not been good this year.)
** Reynald, Pierre, Julian, Sebastian - can you please let us know today
(Thursday in France) if there are any C02-xxx for which a WIYN
observation could be important. If there are any changes to Rob's list,
it should be decided Thursday.
Note that the moon is getting bright - (67% illumination).
Apologies for the short notice,
Tony
"Robert A. Knop Jr." wrote:
>
> WIYN MAY 31 VERSION 1.0
>
> Here's the list of things to observe at WIYN. Candidates are listed in
> the order I think they ought to be done, but feel free to mix-n-match.
>
> Priority key:
>
> A -- we have a spectrum and are following; highest priority to get
> a measurement for stretch purposes.
> B -- we have a spectrum, data for stretch less necessary.
> C -- no spectrum, but has been followed photometrically
> D -- ignore this candidate; why did Rob list it?
>
> d -- ltcv going down as of WIYN May 17
> d! -- ltcv well after max as of WIYN May 17
> m -- ltcv near or just after max as of WIYN May 17
> ??? -- ltcv doesn't make sense; possible errors in fastltcv program?
> or possible errors in TNG data? (Rob: check seeings, xforms)
>
> (Lightcurve information about T02-029 and S02-058 will hopefully come
> in later.)
>
> Mag is a weak-ass magnitude estimate from the May 17 data; typically
> they will be down <~1 mag now. (These magnitudes are hopefully more
> "real" than the discovery magnitude estimates, as they do attempt to put
> in an aperture correction.)
>
> As we're getting later in the lightcurve, "on-color" observations are of
> primary importance to maximize our ability to measure a stretch.
>
> Sunset: 19:31 MST
> Twilight: 21:05 MST
> Twilight: 3:43 MST (6:40 of night; moonrise 0:16 MST)
> Sunrise: 5:17 MST
>
> (Fields get to airmasses of >=2 by morning; press on. I've put the
> brightest candidate at the end and bumped its exposure time.)
>
> Candidate z RA(2000) Dec(2000) Time R(s) Time I(s) Prio Mag
> ==============================================================================
> S02-064 .56 13:25:46.6 +27:34:20.9 4x900 B,d! ~24? (I)
>
> S02-058 13:23:37.3 +27:45:05.1 --- --- D (max ~23) (I)
>
> T02-030 .51 15:43:24.4 +07:53:57.8 3x600 4x600 A,??? 21.9? (R)
>
> T02-028 .44 15:36:25.5 +09:28:18.2 4x900 A,d 23.0 (R)
>
> T02-037 .49 15:46:57.0 +08:12:36.6 3x600 3x900 A,m 22.0 (R)
>
> T02-047 15:36:29.9 +09:38:42.9 4x600 C,m 21.8 (R)
>
> T02-029 .22 15:37:07.5 +09:36:18.7 3x600 3x600 B,m/d 20.8 (R)
>
> -Rob
>
> --
> --Prof. Robert Knop
> Department of Physics & Astronomy, Vanderbilt University
> robert.a.knop@vanderbilt.edu
-- Tony Spadafora ALSpadafora@lbl.gov Physics Division Tel: (510) 495-2316 Lawrence Berkeley National Lab FAX: (510) 486-6738 1 Cyclotron Rd., MS 50-232 Berkeley, CA 94720, USA
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