Short report about the TMR meeting on HDF-S in Padova, June 8-9, 1998 >From the TMR were present: Aragon-Salamanca,Arnouts,Aussel,Bressan,Carraro,Cristiani,De Marchi, Dennefeld,D'Odorico,Franceschini,Longhetti,Petitjean,Silva This was an open meeting, attended by many staff members and young people from Padova,to whom I apologize for not having noted all the names! and also by short term visitors (Alloin, Rampazzo). The meeting was opened by A.Bressan and S.Cristiani, who welcomed the participants. M.Dennefeld stressed the fact that concrete decisions had to be taken before the end of the meeting, concerning the next NTT observations, as well as the scope of future VLT proposals related to this project. The TMR group will concentrate on spectroscopic follow-up, while the imaging is being done mainly by Eso; the participation of Eso staff, invited to the meeting by the TMR collaboration, is regarded as essential, and outlines the spirit of good collaboration between the various groups. The scope of the program of the first day is given below. Dennefeld: Introduction - the general situation of HDF-S D'Odorico: EIS Deep and the HDF-S, FORS-ISAAC capabilities for the follow-up De Marchi: HDF-S observations with VLT Test Camera Aussel: ISOCAM ultra-deep observations of HDF-N and Marano Field Franceschini: ISO observations of HDF-S Arnouts: Photometric reductions, photometric redshifts and clustering in the HDF Nord and South. Aragon-Salamanca: COHSI, the Cambridge OH-Suppression Instrument Carraro: Chemo-dynamical models of elliptical galaxies. Silva: Galaxy Models with dust from UV to the far IR Longhetti: Star formation in field early-type galaxy Petitjean: Characteristics of the HDF-S QSO. Important facts to be retained from those presentations, and the following discussion, are: -The VLT test camera observations will complement the HST observations: deep broad band observations in the Nicmos (U,B,V,R,I) and Stis field (U,I), plus narrow-band Lyman-alpha filter,tuned to z=2.3, in the quasar field and intermediate band imaging for photometric redshift in the WFPC2 field. These observations might be available by end of september,but probably to late for immediate use for the first NTT observations. As a consequence, deep I band images have been requested (and granted) to prepare the multi-object spectroscopy. -The Nicmos3 on HST will give acceptable images in parallel mode,so it is worth considering the follow-up of this field also. -Preliminary ISO identifications are already done, and more should be available at the time of our observations. -Our observations are aiming principally at spectroscopic follow-up,BUT some preselection requires the determination of photometric redshifts. Competitive observations will also be done in Australia. -Ground-based wide-field imaging would be worthwile (e.g. with the new Eso 2.2m camera), specially to study the clustering. It is emphasized also that near-IR colours are important for the redshift range of interest to us,but are not immediately available: Cambridge is planning such a run at Las Campanas with the Cirsi camera,but collaboration may be difficult. Following decisions and recommendations have been taken after extensive discussion: For the NTT observations: -The preliminary imaging in I band scheduled in june should also cover,at least partly, the Nicmos field. (request sent to Eso since the meeting) -Extraction of sources will be done with the help of E.Bertin. -Spectroscopic observations should be limited to a depth allowing coverage of the 3 fields (which means I=~ 21.5),rather then go to limiting depth in only one of them. But deeper spectroscopy will be done around the quasar alone. -Observers will be Dennefeld/Cristiani, at charge to them to prepare the galaxy selection and corresponding masks,which could be done end of August. -Data reduction and release will be an urgent task after observations, for which all necessary forces have not yet been identified. -Contact should be taken with Australia (done in the mean time) and attempt made to coordinate observations as possible. For the VLT proposals: The photometric redshift tool necessary for some preselection is being developped by the Padova group,and selection will be made by them for the TMR group,following requests. Four potential VLT proposals have emerged for the HDF-S: -Spectroscopy of galaxies in the approximate range of z of 1-2.3, selected by photometric redshifts, to look for the peak in SFR. At the same time pick the galaxies responsibles for the QSO absorbtion lines. To be done with ISAAC. Responsible for the draft: Dennefeld/Aragon/Petitjean -Select B drop-outs and follow them spectroscopically. About 10 can be expected in the WFPC2 field, which is as much as already known. To be done with FORS. Responsible for the draft: Cristiani/Charlot(?). -Look for galaxies responsible for the absorbers in the QSO spectrum: follow- up of the NTT proposal, going deeper,but without preselection, specially in the low-redshift (0.3-1) range.Concentrate obviously in the Stis field. To be done with FORS. Responsible for the draft:Petitjean. -Follow-up of Iso candidates. To be done with Fors and Isaac. Responsible of the draft: Franceschini (with Dennefeld and Aussel), and ensure coordination with the corresponding Iso group. The wide-field,visible, follow-up proposal should be drafted by Arnouts. The dead-line for request is the same as for the VLT proposals, but the proposal is independant. The drafts should be circulated by August 17th, so that they can be corrected and presented for final writing and acceptance at the TMR meeting in Leiden early september. Michel Dennefeld