$FORMLOAD_DIR\patt2_sample.dat Sample of a file containing entries to load into the PATT2 Application form to get a sample form Alan Penny Rutherford Appleton Laboratory 1992 Feb Bill Martin Royal Greenwich Observatory 1994 July -------------------------------------------------------------------- 01_1_01#?$& AAT,WHT,INT,JKT,UKIRT !WHT 01_2_01#?$& Semester !95B 01_3_01#?$& Surname of PA !Perlmutter 01_3_02#?$& Title !Prof 01_3_03#?$& Initials !S. 01_3_04#?$& Post held ! 01_3_05#?$& Address (line 1) !Lawrence Berkeley Laboratory,50-232 01_3_06#?$& Address (line 2) !University of California 01_3_07#?$& Address (line 3) !Berkeley, CA 94720 01_3_08#?$& Telephone !1-510-486-5203 01_3_09#?$& Fax !1-510-486-5401 01_3_10#?$& E-Mail !saul@LBL.gov 01_3_11#?$& Will the PA be observing? !Yes 01_4_01#?$& Collaborators (1)-name !R.Ellis, R. McMahon 01_4_02#?$& Collaborators (1)-Inst !IoA 01_4_03#?$& Collaborators (1)-observe? !Yes 01_4_04#?$& Collaborators (2)-name !G. Goldhaber, R. Pain, C. Pennypacker 01_4_05#?$& Collaborators (2)-Inst !LBL 01_4_06#?$& Collaborators (2)-observe? !Yes 01_4_07#?$& Collaborators (3)-name !B. Boyle, P. Bunclark, D. Carter, M. Irwin 01_4_08#?$& Collaborators (3)-Inst !RGO 01_4_09#?$& Collaborators (3)-observe? !Yes 01_4_10#?$& Collaborators (4)-name !A. Goobar 01_4_11#?$& Collaborators (4)-Inst !NOT (Stockholm Univ.) 01_4_12#?$& Collaborators (4)-observe? !Yes 01_5_01#?$& Investigation title(12wds) !High-Redshift Supernova Spectroscopy 01_6_01#?$& Summary of proposal ! \hspace*{0.6in}We have applied for coordinated CFHT and NOAO telescope time to continue the search for high-redshift type Ia supernovae that last year discovered seven SNe Ia at the INT and KPNO 4m telescopes. In the present proposal, we request two nights of spectroscopy on the WHT to study the $>10$ SNe expected from these ongoing searches. These spectra will be used to unambigously establish the SN spectral type and search for evolution effects. These spectroscopic studies are necessary to examine the use of high-redshift SNe as distance-indicators for cosmology, and, in particular, for a first measurement of $q_0$. 01_7_01#?$& Focal station !Cass 01_7_02#?$& Instr and configuration !ISIS, R158B, R158R, 5700 dichroic 01_7_03#?$& Detector(s) !Tek1, Tek2 01_8_01#?$& Time this semester (dark) !2 01_8_02#?$& Time this semester (grey) !- 01_8_03#?$& Time this semester (bright)!- 01_8_04#?$& Specify nights or weeks !nights 01_8_05#?$& Minimum useful (dark) !1 01_8_06#?$& Minimum useful (grey) !- 01_8_07#?$& Minimum useful (bright) !- 01_9_01#?$& Long Term (total time-dark)!- 01_9_02#?$& Long Term (total time-grey)!- 01_9_03#?$& Long Term (total time-brit)!- 01_9_04#?$& Specify nights or weeks !nights 02_1_01#?$& Preferred dates !Sep-Oct following CFHT and NOAO time 02_1_02#?$& Impossible dates !November and later 02_1_03#?$& Justify imp. dates - 1 !galactic lattitude of fields 02_1_04#?$& Justify imp. dates - 2 ! 02_1_05#?$& Other telescopes? Simult? !We have asked that the CFHT and NOAO 3.5m and 4m time be scheduled with ``discovery time'' just before new moon. We request that the 2 WHT nights be in the dark time immediatly following this discovery period. This will allow spectroscopy of SNe at maximum light. 02_1_06#?$& Scheduling constraints ! 02_2_01#?$& Service observing-YES-put-x!- 02_2_02#?$& Service observing -NO-put-x!x 02_2_03#?$& Service observing -maybe x!- 02_3_01#?$& Remote observing - YES x!- 02_3_02#?$& Remote observing - NO x!x 02_3_03#?$& Remote observing - maybe x!- 02_4_01#?$& SA at Tel - every night? x!x 02_4_02#?$& SA at Tel - NO x!- 02_4_03#?$& SA at Tel-first night onlyx!- 02_5_01#?$& List of principal targets ! % \begin{tabular}[t]{p{1.2in}p{1.0in}p{1.0in}p{1.0in}p{1.0in}p{1.0in}} Targets will be determined by the result of the search at CFHT and NOAO telescopes from a list of high redshift clusters around 1 hour R. A. and from fields arranged in slightly overlapping tiles around $ 1^{h} 22.5~{m} +7^{\deg} 15.6^{'} $ % \end{tabular} 02_6_01#?$& Other applications?(Tel)-1 !CFHT 02_6_02#?$& Other applications?(Title) !Homogeneity and Rate of High-Redshift Supernovae 02_6_03#?$& Other applications?(Tel)-2 !NOAO 3.5m and 4m 02_6_04#?$& Other applications?(Title) !Search and Photometric Follow-up of High-redshift Supernovae 02_6_05#?$& Other applications?(Tel)-3 !NOT 02_6_06#?$& Other applications?(Title) !High-Redshift Supernova Light Curve Photometry 02_6_07#?$& Other applications?(Tel)-4 ! 02_6_08#?$& Other applications?(Title) ! 03_1_01#?$& Scientific Justification ! \parbox[t]{7.15in}{ In two observing runs in 1994, we used the INT 2.5m and the KPNO 4m telescopes to discover seven supernovae (SNe) at redshifts between $z$ = 0.3 and 0.5. These discoveries confirm estimates of distant Type Ia SN rates, and prove the capability of our search technique to find high-redshift SNe on demand just before new moon. Every SN discovered was followed through its lightcurve with photometry (see Figure 1), and with spectroscopy of the SN and/or its host galaxy (see Figure 2). [NB: The final, calibrated host galaxy images without the supernovae have been observed in the past few months (not shown in Figure 1); these images were necessary to complete the light curve analyses for publication.] \vspace{.12in} This proposal is for a complementary spectral study of high-redshift type Ia supernovae. The SNe Ia will be discovered in a search that continues the techniques (see Technical Information) developed in the past few years by our team, using coordinated time at the INT and NOAO telescopes (e.g., Perlmutter et al, {\em Ap.J.Lett.}, 440:L41, 1995). However, this next semester's continuation of the search will be coordinated at the CFHT and NOAO telescopes, to take advantage of wider-field cameras and better seeing. Scaling from the seven SNe discovered in our previous searching, we should find $>10$ supernovae at each site. Our high-redshift SN work at the INT will resume when the INT Wide Field CCD camera becomes available. \vspace{.12in} The remarkable homogeneity of the light curves and spectra of nearby ``normal'' SNe Ia, together with their visibility to high redshift, potentially makes them uniquely suited to measuring the decelleration parameter $q_o$. The measured dispersion in absolute magnitude for nearby Type Ia SNe that are not reddened or intrinsically red ($B-V > 0.3$) is approximately $\sigma_{M_B} = 0.3$ mag (Vaughan et al, {\em Ap.J.}, 439:558, 1995). This dispersion is completely accounted for by the measurement errors; Sandage and Tammann ({\em Ap.J.}, 415:1, 1993) suggest that the intrinsic dispersion is less than 0.2 mag. Including the rarer, redder --- and spectroscopically ``peculiar'' --- SNe ($\sim$15\% of the Type Ia's) gives a higher measured dispersion, however Hamuy et al ({\em A.J.},109:1, 1995) has shown a correlation with lightcurve decay time that may allow these SNe to be calibrated to give an even smaller dispersion of 0.1 mag. For $\sim$12 SNe at $z = 0.5$, a conservative intrinsic dispersion of 0.25 mag would give a formal uncertainty in $q_o$ of $\sigma_{q_o} = 0.15$. This is a statistical accuracy as good as the best previous measurements of global curvature, but without the galactic evolutionary errors. \vspace{.12in} We propose to use the WHT to obtain spectra of our SNe as close to maximum light as possible. Apart from providing redshift information, this spectroscopy study will address two main questions that test the use of Type Ia SNe as ``standard candles" for cosmology: (1) Are the supernovae we discover ``normal'' SNe Ia, or do their spectra match the ``peculiar'' SNe Ia (such as SN 1991T, SN 1991bg, and SN 1986G) that appear to have non-standard absolute magnitudes. This will be important in determining the dispersion of absolute magnitude at maximum light for ``normal'' high-redshift Type Ia's. The confirmation of spectroscopic ``normal'' SNe Ia among the supernovae discovered this next semester should make it possible to make a measurement of $q_0$ using this supernova sample. (2) Are high-redshift Type Ia's otherwise spectroscopically similar to nearby Type Ia's? Spectra near maximum light will give a first-order test of this similarity, and provide an indicator of evolutionary differences. \vspace{.12in} In addition, we propose to obtain high quality spectra of four of our present set of supernovae host galaxies, now that the supernovae have faded. We will use these spectra to complete the studies of the supernova spectroscopy to discriminate between the host galaxy features and any evolutionary changes in these supernovae. (The time-critical supernova spectra will, of course, be completed at higher priority than the host galaxy spectra.) } 04_1_01#?$& Technical information (I) ! \parbox[t]{7.25in}{ It has traditionally been very difficult to schedule large telescopes to observe SNe at their maximum light, and during dark time, since they are normally discovered at random times. The problem is compounded for high-redshift SNe, since 4-meter class telescopes are required. Our solution to this problem is to discover high-redshift supernovae in batches. The basic idea is to observe many reference fields during a week just past new moon, and then re-observe these fields two weeks later just before the next new moon. This yields a group of supernovae almost all discovered before maximum and all visible during the following dark (new moon) nights for {\em scheduled} follow-up spectroscopy and photometry. As in our previous work at the INT, we will use this search approach in the coordinated CFHT and NOAO telescope time that will find the supernovae to be observed with this current proposal's time. \vspace{.12in} Also as in our previous work, the supernovae will be found using next-day automated image comparisons. The data is transmitted over the networks to Berkeley, where a team of scientists and students can analyze the data while the observers sleep. This approach has made it possible to detect the SNe within 24 to 48 hours. The Berkeley team prepares finding charts and estimates observing times and recommended slit position angles, and coordinates the follow-up observations at the telescopes by phone and e-mail. \vspace{.12in} The supernovae that will be studied spectroscopically by this proposed time will also be followed with photometry throughout their light curves at a number of telescopes located in uncorelated weather sites around the world. The photometry sites include WIYN (Perlmutter et al), NOT (Goobar et al), ARC (York), SSO (Mould et al), and Cananea, Mexico (Carrasco), all 2-meter class telescopes or larger. The telescope coverage for spectroscopy is less complete, since it requires a 4-meter telescope; besides this WHT proposal, we are applying for two Mauna Kea telescopes, Keck (with Filippenko) and CFHT (as part of the coordinated search). Given the resources devoted to finding the supernovae, and following the photometry, the WHT will thus play a crucial role in the spectroscopy. \vspace{.12in} The spectrum of one of our KPNO discoveries, SN 1994G, was obtained in 2 hours on the MMT (see Figure 2), with most of the better signal-to-noise data from 1 hour. Therefore the 2 nights requested for WHT spectroscopy should be just barely sufficient to study $\sim$10 SNe, accounting for calibration and standard stars. } 04_1_02#?$& Technical information (II) ! \parbox[t]{7.25in}{ } 05_1_01#?$& Backup programme (summary) ! Spectra of the host galaxies of 4 high-redshift supernovae discovered by this project this past year. 05_2_01#?$& Last 4 Sems (see,eg,Table) ! \begin{tabular}[t]{p{1.5in}p{0.7in}p{0.8in}p{3.2in}} 1/W/ & 0 & & \\ 1/X/ & 0 & & \\ 1/Y/ & 2 weeks & 8 nights & and 2 nights with seeing $> 3"$ \\ 94B/ & 2 weeks & $<$4 nights\\ 95A/ & 0 & &\\ \end{tabular} 05_3_01#?$& Pubs for last 4 Sems (6) !Perlmutter, S. et al.,'A Supernova at $z = 0.458$ and Implications for the Cosmological Deceleration', 1995, Ap. J. Lett., 440:L41.\\ Perlmutter, S {\it et al}, IAU Circ. 5956 and 5958 \\ Further publications are now in preparation. As mentioned in the Scientific Justification, the final, calibrated host galaxy images without the supernovae have been observed in the past few months; these images are necessary to complete the light curve analyses for publication. Thus there is always at least a year delay between discoveries and publications. 05_4_01#?$& Experience of Observers !All experienced users 05_5_01#?$& Student research? (Name) ! 05_5_02#?$& Student research (Grant) ! 05_6_01#?$& Research grant obs? (PI) ! 05_6_02#?$& Research obs?(Grant title)! 05_6_03#?$& Research obs? (Grant No.) ! 05_7_01#?$& Non-standard T and S ! 05_8_01#?$& Other expenditure(freight)! 06_2_01#?$& Summary Slip (short title)!High-redshift Supernovae Spectroscopy 06_2_02#?$& Pricipal App and Institute!Saul Perlmutter, LBL 06_2_03#?$& Time this Semester (Dark) !2 06_2_04#?$& Time this Semester (Grey) !- 06_2_05#?$& Time this Semester(Bright)!- 06_2_06#?$& Time requested(nights/wks)!nights 06_3_01#?$& Acknowledge (short title) !High-redshift Supernovae Spectroscopy 06_3_02#?$& Address for Acknowledge ! Saul Perlmutter\newline Lawrence Berkeley Laboratory 50-232\newline University of California \newline Berkeley, CA, 94720. XE_0_00#?$& LaTeX setup commands p! \font\frmin=cmr7