Date: Tue, 2 Jul 2002 21:10:16 -0500 From: Donald G. York To: elt@astro.Princeton.EDU, wall@orca.astro.washington.edu, stubbs@welkin.astro.washington.edu, kurt@nmsu.edu, tsnow@origins.colorado.edu, pdf@pha.jhu.edu, al@hale.yerkes.uchicago.edu, jtl@oddjob.uchicago.edu, jtl@elvis.astro.nwu.edu Subject: A modest proposal This last quarter, I proposed to the UC Tac that we take one half night each week, on Friday night, to observe transient sources that are not of a nature to warrant interrupting the entire APO 3.5m schedule (such as gamma ray bursts) but which do gain from regular, weekly monitoring. The Friday night request was to enable observing from Adler for an exteneded period, when the public can view work with a large telescope. The observer would do his/her work and an interpreter would be present to handle the public. When the Adler closed for the (late) evening, the observations would move to UC campus for completion, if arrangements could not be made to stay at Adler. The proposal is attached. I am sending to someone from each institution who I know might be interested in joining this effort. The idea would be as follows: each TAC ranks internal proposals for use of such time very high (to enable Ed to schedule a particular night and first half with priority over other requests. Each institution puts in an amount of time proportional in some way to the no. of minutes actually spent on their targets. One person manages requests from all institutions, based on a monthly phone con of the key parties. Nothing would be observed that was not in the proposals submitted. One time events not thought of would remain director's discretion. For special cases, this rule could be violated, but only with written permission from the TAC chair at the requesting institution and the 3.5m director or his/her designee. (I put this in to remove an obvious objection. If it is too restrictive, we can modify it. It is, however, the rule I intend to live by. PLease help me get this mail to the correct person at each institution. If anyone wants to be a part of it and, in particular, be the lead for an institution, I would like to hear from them. The targets will change each quarter, of course, depending on how well each program works and which ones get taken to completion. On this plan, the coordination comes in two ways. 1) We should all agree on a buzz word that we put in our titles, so Ed knows that a common program is envisioned by the respective tacs. 2) In a monthly meeting, the weekly observing lists would have to be prioritorized. Presumably, each lead contact would take a turn at that monthly coordination. I am willing to do it for the three months of Quarter 4, 2002, but am also willing to have it rotate monthly if volunteers show up. I cannot do it in the Winter and Spring, 2003, but am available again for Q3 and Q4, 2003. NOte that in the event targets are sparse on a given evening, an accepted, different program, would use the time. I doubt this will occur much, but it should be written in to cover the eventuality. FORM2.UC DATE:May 16, 2002 INSTITUTIONAL ID NUMBER: DESCRIPTIVE TITLE: Weekly Observations of Transient Sources FACULTY SPONSOR (= PI): Donald G. York SIGNATURE: ___________________________ OBSERVER(S): Don York, Lucy Fortson, Geza Gyuk, Mark Hammergren, Don Lamb , Jonathan Mitchell, James Lauroesch The faculty sponsor CERTIFIES that the observer(s) listed above is qualified to use the telescope: ( X )Remotely , (X )Alone On-Site , ( )On-Site when accompanied by the sponsor . L. Fortson needs to be trained. (Others will be involved in data analysis, especially for the SNe program--Hobbs, Jenkins, Bowen.) EMAIL ADDRESSES of faculty sponsor and of at least one UC observer (if any): don@oddjob.uchicago.edu, jmitchell@orbit.adler.uchicago.edu List < 4 PUBLISHED PAPERS (yr, journal, vol, pg), not necessarily your own, which describe important work on this topic: Noble et al, 2001. Meteoritics and Planetary Science 36, 31 (regolith on asteroids.) Costamante and Ghisellini (A&A 384, 56 (2002) (TeV bursts) Morton, York and Jenkins 1986, ApJ, 302, 272. (Extent of ionized Ca in galaxies.) List < 3 PUBLISHED PAPERS (yr, journal, vol, pg) of your own on this topic: Yanny, York and Gallagher 1989, ApJ, 338, 735 Jenkins, Rodgers, Harding, Morton and York 1984, ApJ, 281, 585. THESIS OBSERVATIONS ? Y______ N___X___ Is this a CONTINUATION of a previous program ? Y_____ N__x____ UC ID number: Title: NA Faculty Sponsor: Observer(s): York and others. Most recent observing time (month/yr): Total OBSERVING HOURS requested (with a separate section for each instrument): Instrument: Echelle, DIS, GRIM, SPICAM, with the relative amounts of time contingent (depends on matters arising) Total hours: 20 Preferred dates: Friday, first halves Excluded dates (scientific): None Excluded dates (personal): None List < 7 of your most important TARGETS [name, approx. RA, approx. DEC, V (or other relevant) magnitude]: source RA(2000) Dec(2000) Vis mag Program 1ES 1959+650 19h59m59.8s +65d08m55s 14.7 Tev flares 1ES 2344+514 23h47m04.8s +51d42m18s 15.5 Tev flares RGB J1725+118 17h25m04.3s +11d52m15s 15.8 Tev flares 0235+167 02h38m39s +16d36m59s 15-20 HST targ. of op. small asteroids 2-3 at any one time over season 20 meteorite/asteroid NEO 1/mo. 21 orbits for small NEOs Supernovas one per mo. <14 echelle, IS lines in host Briefly describe any expected FUTURE REQUESTS for observing time for this program: We expect to make this a continuing program, in conjunction with the public observing opportunity, weekly, at Adler. Since we need to pick a particular night of the week for long term scheduling, we choose Friday, when the Adler members of this proposal can do the observing from Adler. This program will enhance the opportunities for science outreach, in parallel with a new science opportunity for APO. Briefly describe (yr, # hrs, brief program title, resulting publications) all AWARDS OF 3.5M OBSERVING TIME, within the last 2 years, to the faculty sponsor listed above: Yr Hrs Title (Publications-see footnotes, below) Assigned Useful -- --- -------------------- 00/Q2 ?* ? DGY Adler 00/Q2 24 12 DGY *Diffuse Interstellar Bands 00/Q2 24 15? DGY, BW **FP, em. from QSOALS 00/Q3 24 4 DGY, Oka + DIB in really reddened stars 00/Q3 20 10 DGY,H, O, M * Diffuse Interstellar Bands 00/Q3 22 12 DGY, VK +++Damped Ly Alpha in published SDSS QSOs 00/Q3 18 7 DGY, CM ++HVCs in RR Lyr stars 00/Q4 41 19 DGY, CM ++HVCs in RR Lyr stars. 00/Q4 43 20 DGY, VK, BW **FP , emis. from QSOALS 00/Q4 43 26 DGY, H, O, M *. DIBs 01/Q1 50 6 DGY, H, O, M *. DIBs 01/Q1 40 -- DGY, VK, BW **FP , emission from QSOALS 01/Q2 48 20 DGY, VK, BW **FP , emis. from QSOALS 01/Q2 77 52 DGY, TO, BM *DIBs 01/Q3 13 13 DGY, TO, BM *DIBs 01/Q3 20 15 Oka, York, ... + C3 in really reddened stars 01/Q4 55 20 DGY, TO, BM *DIBs 01/Q4 50 16 DGY, VK, BW **FP 02/Q1 45 21 DGY, TO, BM *DIBs (5 hours taken as open time) 02/Q1 40 20 DGY, VK, BW **FP 02/Q2 48 -- DGY et al. *DIBs (this proposal), upcoming in May, June 02/Q2 40 8 DGY, VK, BW **FP + Observations to define DIBs in very reddened stars and search for C3. 2002, Oka, Thorburn et al. Paper ready to submit. Observations of C3 in Translucent Clouds Oka, T., Thorburn, J. A., McCall, B. J., Friedman, S. D., Hobbs, L. M., Sonnentrucker, P., Welty, D. E., York, D. G. 2002, ApJ (second draft done) ++Observations of high velocity clouds using RR Lyr stars. On hold until Mallouris finishes his thesis (Q1, 2002) +++On hold until we have a better SDSS line list. **Long term, FP imaging of high z galaxies. Reductions are done for all data taken. We await completion of very long exposures (by averaging 40 min. exposures, on our objects.) *Long term, DIB proposal. Observations of Diffuse Interstellar Bands Attributed to C7- McCall, York, Oka, 2000, ApJ,531, 329. Rejection of C7- as the Source of the Diffuse Interstellar Bands. McCall, Thorburn, Hobbs, Oka, York, ApJ Letters, 559, L49. 1. A Critical Examination of the l-C3H2- Spectrum and the Diffuse Interstellar Bands McCall, B. J., Oka, T., Thorburn, J., Hobbs, L. M. and York, D. G., 2002 ApJ, 567, L145. Unusually Weak Diffuse Interstellar Bands toward HD 62542. Snow, T. P., Welty, D. E., Thorburn, J., Hobbs, L. M., McCall, B. J., Sonnentrucker, P., York, D. G. , 2002. ApJ, in press. Diffuse Interstellar Bands Associated with High C2 Column Densities Thorburn, Oka, Hobbs, McCall, Welty, Snow, Friedman, Sonnentrucker, Rachford, York (2nd draft complete) Correlations of Diffuse Interstellar Bands, presented by McCall, Conference on Lab Astrophysics, Ames, 04/02 Relation of H2 to the Diffuse Interstellar Bands, presented by York, FUSE conference, March 21, 2002. We obtained 6 hours in February of Director's Discretionary time to obtain spectra of SN2002ap. GCN SN2002ap report Echelle spectrum of SN2002ap at 0H UT, 02/08/02 Lamb, D. Q., Lauroesch, J. T., York, D. G., Hastings, C., Bowen, D. V., Meyer, D. ADDITIONAL COMMENTS: The program is to observe targets of opportunity that can benefit from weekly, short observations, using a permanently scheduled half-night, on Fridays. Examples of current programs to be pursued are listed below. Operationally, the group will have a phone call each Wednesday, to agree on the targets that should be done the next Friday and to make observing assignments. The lead person for the week (York will be the default individual) will then mail obs-spec to give the desired instrument change plan and get concurrence from APO. We expect the plan to evolve as we get experience. Our plan is to list the programs in each quarter that we plan to pursue that quarter, so that all observations have been approved by the TAC and by the Director. It may happen that other opportunities arise and that we will seek permission for new objects on short notice. In that case, if permission is granted, the data will be available to all ARC scientists, and/or we will comply with whatever rules are deemed appropriate. In the event that no objects are available ( not likely), York will use the time for an accepted APO science proposal. In later quarters, we expect other institutions to join this effort. York has talked to E. Turner, who is supportive and may ask Princeton to support this proposal this quarter. For this quarter, the Adler activity for the public is not in session (summer nights are too short). That aspect of the program would begin if we obtain time in the Fall. We will use the summer to gather experience on optimal scheduling techniques and to define logistical problems. SCIENTIFIC JUSTIFICATION AND SUMMARY OF PROGRESS: I. Overview and Summary We propose a long term assignment of one-half night per week, to be applied for quarterly, of the 3.5 meter telescope to monitoring programs that will benefit from once a week monitoring. Such proposals are currently awkward to schedule, once the typical targets of opportunity arise, because the exposure times are short and the number of time trades (or, really, periods when the prime observer would just give up the time) is too large (for the Director and for the observers and for the staff at APO.) We request the time to be weekly, the first half of Friday night. This scheduling will allow the Adler partners to observe from Adler and to extend the public observing time from the pre twilight hours, into the night. (Logistically, this program will require three staff in Chicago--an Adler observer; an observer ready to take over from the campus of The University of Chicago, once Adler closes for the night (seasonally variable); and a public interpreter at Adler, so the Adler observer can concentrate on the program. Our large team will cover these positions. We would hope that other ARC institutions would contribute time and take advantage of the opportunity to add targets that fit the special requirements of this program. Ed Turner can combine these similar proposals once he gets the departmental requests, quarterly. For this inaugural proposal, we propose as targets: small asteroids, to establish the similarity of asteroids and meteroites; faint, near Earth objects (NEOs) that are normally "lost" before an orbit is obtained; monitoring of AGNs to establish a link between optical/IR flux and TeV flares in the same objects; supernovas brighter than magnitude14th, to study the interstellar material in the host galaxies; and an AGN (BL Lac) that we need to catch a peak brightness to schedule an HST spectroscopic observation of intergalactic zinc. II. Science Program Justifications A. Reflectance Spectroscopy of Very Small Near-Earth Asteroids (Hammergren, Adler) Reflectance spectroscopy is a well-established tool for the remote determination of solid-body composition, and has been successfully applied to the study of asteroids (Binzel et al, 1996. Science 273, 946). Perhaps the greatest outstanding problem in planetary science is identifying the connection between meteorites and asteroids, their presumed parent bodies. Most work on this topic has been done using reflectance spectroscopy to identify spectral analogs of meteorites among the asteroids. Here, a complicating factor appears to be "space weathering", a disguising process which causes rocky materials to darken, redden, and lose contrast in their spectral absorption bands when exposed for long periods to the space environment. Studies of lunar materials have revealed that space weathering is almost certainly due to the generation of nanoscale reduced iron particles on the exposed surfaces of mineral grains (Noble et al, 2001. Meteoritics and Planetary Science 36, 31). Since it is a surface process, its optical effects are promoted in loosely compacted particulate layers. Laboratory simulations using ground-up meteorites have produced this same space weathering effect on presumed asteroidal material (Sasaki et al, 2001. Nature 410, 555). It has been found (Pravec and Harris, 2000. Icarus 148, 12) that the majority of asteroids smaller than about 200 meters diameter rotate faster than the gravitational binding limit. Such rapidly rotating asteroids are necessarily free of regolith, and are the only ones for which we can be certain we are seeing bare rock. Space weathering is therefore much less of a concern on these bodies. There are extensive monitoring programs that will discover the appropriate, small asteroids. There will be 2 or 3 available each week. Because of its relatively large aperture, its ability to accurately track at rapid non-sidereal rates, and the wide wavelength coverage of DIS, the ARC 3.5-m is very well suited for the spectroscopy of these near-Earth, <200 meter asteroids. An earlier program of asteroid spectroscopy (Hammergren, PhD thesis) proved that it was possible to obtain useful DIS spectra of 19th magnitude asteroids with 15-minute exposure times. Additional spectra of bright (8 to 9th magnitude) solar analog stars at comparable airmasses are required to remove the solar continuum. B. Astrometric Follow-up of Faint Near-Earth Objects (Hammergrean, Adler) NASA has identified as a top priority for its Near-Earth Object (NEO) program the discovery and orbit determination of near-Earth asteroids. Almost all NEOs are discovered by telescopes smaller than 1.2 meters in aperture, and the majority of astrometric follow-up is performed by amateur astronomers using telescopes with apertures of less than 0.5 meters. As a result, NEOs are often considered to be "lost" if follow-up observations have not been performed before the objects have faded below 21st magnitude. Objects at the 22 mag level can still be large enough to cause significant damage on Earth. These numerous objects are currently not followed up on. There will be about one per month and the total observing time on each will be ~15 minutes (Spicam). The ARC 3.5-m would be the largest telescope in the world at which asteroid observations would routinely be performed, and would be a unique resource for extending the timespan over which newly discovered NEOs are observed. The corresponding improvement in NEO orbits will allow them to be found more easily at future oppositions, which is necessary for precise orbit determination. This proposed use of the ARC has the potential to attract considerable attention from the scientific community and the general public, if our observations should (presumably) eliminate an impact hazard. Again, the ability of the ARC 3.5-m to accurately track at rapid non-sidereal rates makes the ARC/SPICam system particularly well suited for faint NEO followup. In the proposed observing scheme, the telescope would be driven at the predicted rate of motion of the asteroid, and background stars would be trailed. Exposure times (SPICAM) would be limited by either sky brightness or the open-loop tracking ability of the telescope. A short sequence of two or three exposures would be sufficient to eliminate spurious detections. C. AGNs and TeV Flares (L. Fortson, Adler/UC) Some bright AGNs are known to be TeV flare objects. The timescales are poorly known, and there are both DC increases and sporadic, flare increases. Recent work by Costamante and Ghisellini (A&A 384, 56, 2002), hereafter GS02) provides a list of BL Lacs which are TeV candidate emitters. Their selection was based on a comparison of the X-ray flux as a function of (i) radio flux (ii) optical flux. They proposed that the radio flux may measure the level of the relevant seed photons available for Inverse Compton scattering. If this is the case then for a given X-ray flux, sources that are brighter in the radio band are more likely to be TeV emitters. However, as the seed photons most effective for the TeV emission are in the IR-optical band, the optical/IR flux could be a better indicator of the density of seed photons than the radio flux. From their studies, GS02 concluded that for a given X-ray flux, a relatively high emission in both the radio and optical-IR bands should represent a reliable indication of a large density of seed photons. A remaining question is whether we can use this model to understand flaring in these objects. By continuous monitoring of optical-IR activity in the candidate objects before the object is detected by flaring in the TeV, we might be able to obtain correlations that allow us to predict which types of candidates are likely to flare into the TeV region. TeV flares cannot be detected with high sensitivity at this time. However, a new project, VERITAS, promises to greatly enhance the sensitivity. An understanding of any predictive indicators of TEV flares will have a major impact on the science of VERITAS. D. Interstellar Matter in Host Galaxies of Supernovae D. York, J. Lauroesch, D. Lamb Supernova brighter than 14th magnitude are now discovered monthly. Echelle spectra of these opportunities, in the first two weeks of their lives, provide an opportunity to obtain information on interstellar gas in the host galaxy of the supernovas. [For instance, echelle observations of Supernova Evans in M83(1983), Jenkins, Rodgers, Harding, Morton and York 1984, ApJ, 281, 585, showed a much higher velocity dispersion for interstellar Ca II lines in M83, compared to those in halo sightlines of our own Galaxy, consistent with the ~5 times higher SN rate in M83 compared to the Milky Way (since supernova energy stirs the interstellar medium and moves the clouds around.)] Since the SNe occur in different parts of galaxies, the technique allows the sampling of interstellar path lengths not otherwise available. Generically, the experiment accomplished is similar to that done with QSO absorption lines, except that in this case, the galaxy itself is well seen and the potential for physical understanding of the material is higher. Only a handful of such opportunities have ever been taken advantage of by large telescopes, because of the need to have the correct instrument and an interested scientist at the telescope when the rare opportunities occur. The easy change to the echelle and the availability of remote observing make this obsevation much easier with the 3.5 meter telescope. In March, 2002, we (with Meyer, Bowen and Wallerstein) obtained time, 2 hours for each of three weeks, to catch SN2002ap, in M74, at peak, and record echelle spectra. On our first night, the object was at 14th magnitude. We found the (very narrow) interstellar lines, proving the efficacy of this program. We took 5, 15-minute exposures and co-added them to get the result. Narrow Na I from the host was detected (redshift 650 km/sec), while two Ca II components, covering 100 km/sec, were found (probably, intermediate velocity gas with Routly Sptizer effect, as one would find in our own Galaxy.) A GCN was filed, by Lamb, et al. A second SN was attempted by Wallerstein, a few weeks later, with positive results in terms of echelle sensitivity. However, the data were affected by moonlight. E. AGN monitoring for HST Targets of Opportunity V. Kulkarni, J. Lauroesch, D. York The indicated group, with Welty (UC) and M. Fall (STScI), have been assigned HST time to measure the abundance of zinc in intergalactic absorption lines, using QSOs as the background sources, with high resolution STIS spectra. We are focusing on the abundance in QSO absorption line systems that are at redshifts below 0.4, in the regime for which models predict the zinc should begin to reach solar values (it is always well below solar in the better studied systems at high z). There are very few systems available, but one of the best is the BL Lac/QSO 0235-167 (Yanny, York and Gallagher 1989, ApJ, 338, 735.) The object is usually fainter than 18th magnitude, but can flare to 15.5 magnitudes, for a month at a time. HST has given us target of opportunity status. We need to monitor the source weekly and notify HST when it is bright. We propose to monitor the object weekly, using whatever instrument is on the telescope at a given time, using the appropriate imaging device (DIS guiders, echelle guider, SPICAM, etc.). The program will end once we catch the bright state and the HST observation is scheduled. (This is an example of many types of observations that will be done under this program, which require monitoring to catch the object in the brightest state, to be followed up by satellite observations. As far as we can tell, the other AGN monitoring programs are not hitting this object frequently enough for our purposes. While it could be done with a smaller telescope, it is trivial to insert it into this larger program.) INSTITUTIONAL ID NUMBER: DESCRIPTIVE TITLE: Weekly Observations of Transient Sources PI: Donald G. York The University of Chicago don@oddjob.uchicago.edu OBSERVER(S): Don York, Lucy Fortson, Geza Gyuk, Mark Hammergren, Don Lamb , Jonathan Mitchell, James Lauroesch UNCERTIFIED/UNTRAINED OBSERVERS: L. Fortson needs to be trained, which York will do. COLLABORATORS: Don York (don@oddjob.uchicago) Lucy Fortson (lucy@cynus.uchicago.edu) Geza Gyuk (gyuk@oddjob.uchicago.edu) Mark Hammergren ( mhammergren@orbit.adler.uchicago.edu) Don Lamb (lamb@oddjob) Jonathan Mitchell (jmitchell@orbit.adler.uchicago.edu) James Lauroesch (jtl@oddjob) CONTACT INFORMATION: don@oddjob.uchicago.edu, 773 702 8930 HALF NIGHTS OR HOURS REQUESTED: 20 hours INSTRUMENT: Echelle, DIS, GRIM, SPICAM, contingent on targets of opportunity PRIMARY DIS GRATING: NA SECONDARY DIS GRATING (IF REQUIRED): NA SLITS/FILTERS/ETC NEEDED: OBSERVING MODE: Remote OBSERVING SCHEDULE CONSTRAINTS: Requesting Friday nights, to be in conjunction with public nights at Adler, and extension of the pre-twilight program already going on. SPECIAL REQUIREMENTS: First halves only. TARGET LIST (selected stars, full range of coords.) source RA(2000) Dec(2000) Vis mag Program 1ES 1959+650 19h59m59.8s +65d08m55s 14.7 Tev flares 1ES 2344+514 23h47m04.8s +51d42m18s 15.5 Tev flares RGB J1725+118 17h25m04.3s +11d52m15s 15.8 Tev flares 0235+167 02h38m39s +16d36m59s 15-20 HST targ. of op. small asteroids 2-3 at any one time over season 20 meteorite/asteroid NEO 1/mo. 21 orbits for small NEOs Supernovas one per mo. <14 echelle, IS lines in host SPECIAL PROTECTION JUSTIFICATION: None BRIEF SCIENCE JUSTIFICATION: There are a number of scientific observations that require periodic sampling for very short periods of time at each exposure. The APO 3.5 meter telescope is well set up to do several small programs on a single night, using different instruments. However, the scheduling burden for numerous short programs on targets of opportunity is heavy. We propose to use one-half night each week (first half of Friday night) to observe objects preapproved for such purposes. After this first quarter, the observing will be done at Adler in conjunction with the public outreach program that is already on going there with the 3.5 meter telescope. For this quarter, we are focusing on five types of observations: a) DIS observations of small asteroids (<200 meters in diameter) that are spinning too fast to have an aged coating. The reflectance spectrum of these fresh surfaces will be used to relate asteroids to the meteorites that hit Earth. Two or three will be available each week. The DIS observations will require 15-30 minutes each. b) Faint near Earth objects (NEOs) may be on collision paths with Earth. The brighter of these are well monitored, for which cases amateur followup on small telescopes are adquate. However, the smaller, fainter objects, near magnitude 21, require followup with a big telescope, to determine orbital elements and to rule out the "impact orbit" solution. About one a month is expected to be available. The SPICAM observations will require less than 1/2 hour. c) Some AGNs are TeV flare sources. With the advent of VERITAS, higher sensitivity to detecting these flares will be available. A predictive algorithm is needed. Based on one model, the IR/optical flux may be a good indicator of impending TeV flare activity. Several TeV flare sources will be monitored weekly in three colors to see if the flares (assumed eventually to occur, since they have in the past) have progenitor activity in the optical IR associated with them. d) One AGN/BL Lac, 0235+167, is on our target list for HST observing with STIS. While it has excellent prospects for providing a definitive measure ofthe zinc abundance in the Universe at z~0.5, the object spends most of its time in a low state, too faint for observation by STIS. It does become bright enough to observe for a few weeks at a time. We will monitor it weekly to catch it in a high state and implement an approved HST target of opportunity observation. e) Supernovae innear by galaxies reach magnitude 14 or less, and are suitable for studies of the interstellar medium in the host galaxies. The resulting interstellar Na I and Ca II lines can be used to describe the interstellar medium and reflect the star formation rate (through the velocity dispersion of gas clouds initiated and maintained by mechanical energy from the supernova shocks). We will obtain spectra of all suitable SNe for this purpose. PUBLICATIONS BASED ON APO 3.5m DATA: 1. McCall, B.J., York, D.G., and Oka, T. 1999. Observations of Diffuse Interstellar Bands Attributed to C7-, Astrophysical Journal, 531, 329. 2. White, R...., Richards, G. 2000, FIRST QSOs, ApJS, 126, 133 (York time) 3. Fan et al. 2000. SDSS Quasars from Commissioning, Astronomical Journal, 119, 1. Zheng et al, 2000, Five new QSOs..., AJ 120, 1607. 4. Yanny, B. et al.2000, Identification of A stars in the Halo, ApJ, 540, 825. 5. Richards, G. T. 2000, Absorption Line Properites of z~2.5 Radio Sources, Ap J S, 133, 53. (York time). 6. Richards, G. T., Laurent-Muehleisen, Becker and York, 2001, ApJ, 547, 635. (York time) 7. Anderson, S. F., Fan., X., Richards, G. T., ...and York, D. G. 2001, High z QSOs, z>4, confirmed on 3.5m. 2001, A. J., 122, 503. 8. McCall, B. J., Thorburn, J., Hobbs, L. M., Oka, T., and York, D. G. 2001, Rejection of the C7- Diffuse Interstellar Band Hypothesis. Ap J Letters, 559, L49. 9. Fan et al , A Survey of z>5.8 Quasars in the Sloan Digital Sky Survey I..., AJ, in press. 10. Geballe et al, spectra of brown dwarfs, in press (December, 2001 publication.) 11. Snow, T. P., Welty, D. E., Thorburn, J., Hobbs, L. M., Oka, T., McCall, B. J., York, D. G. and Sonnentrucker, P., 2002. Unusually Weak Diffuse Interstellar Bands toward HD 62542. Astrophysical Journal, in press. 12. McCall, B. J., Oka, T., Thorburn, J., Hobbs, L. M. and York, D. G., 2002. A Critical Examination of the l-C3H2- Spectrum and the Diffuse Interstellar Bands. Astrophysical Journal Letters, ApJ, 567, L145. *****************(not yet refereed)********************************** Correlations of Diffuse Interstellar Bands, presented by McCall, Conference on Lab Astrophysics, Ames, 04/02 Relation of H2 to the Diffuse Interstellar Bands, presented by York, FUSE conference, March 21, 2002. Oka, T., Thorburn, J. A., McCall, B. J., Friedman, S. D., Hobbs, L. M., Sonnentrucker, P., Welty, D. E., York, D. G. 2002, Observations of C3 in Translucent Clouds. ApJ (second draft done) Diffuse Interstellar Bands Associated with High C2 Column Densities Thorburn, Oka, Hobbs, McCall, Welty, Snow, Friedman, Sonnentrucker, Rachford, York (2nd draft complete) GCN SN2002ap report Echelle spectrum of SN2002ap at 0H UT, 02/08/02 Lamb, D. Q., Lauroesch, J. T., York, D. G., Hastings, C., Bowen, D. V., Meyer, D.