The ESO Large Programme 185.D-0056 (HARPS@3.6m) continued in June and July 2011, with the first radial velocity survey of red giants. The log of the the observations, the problems encountered, some tips in the use of HARPS in the HAM mode, the situation of the publications, and a look to the future are given

Hareter, M

MANTEGAZZA, Luciano Romolo

PORETTI, Ennio

RAINER, Monica

OA@INAF - Istituto Nazionale di Astrofisica

2011Publication Year2023-02-24T09:00:41ZAcceptance in OA@INAFReport on the third run of the ESO LP 185.D-0056 (HARPS@3.6m)TitlePORETTI, Ennio; Hareter, M; MANTEGAZZA, Luciano Romolo; RAINER, MonicaAuthorshttp://hdl.handle.net/20.500.12386/33807Handle10NumberReport on the third run of the ESO LP 185.D-0056(HARPS@3.6m)E. Poretti, M. Hareter, L. Mantegazza, and M. RainerSeismology Ground-Based Observation Working GroupOctober 27, 2011; Version 1.0EXECUTIVE SUMMARY.The ESO Large Programme 185.D-0056 (HARPS@3.6m)continued in June and July 2011, with the first radial veloc-ity survey of red giants. The log of the the observations, theproblems encountered, some tips in the use of HARPS in theHAM mode, the situation of the publications, and a look to thefuture are given. The following actions/items are emphasized:1. the observations were devoted to the red giants in theopen cluster NGC 6633 using the HAM configuraton. Afew other CoRoT targets belonging to other pointings wereobserved;2. the first 10-nights run had excellent weather conditions,with just one night lost; the second 5-nights run was moredisturbed, with only 2 good nights;3. different filling programmes were run at the beginning andend of night.4. we had no technical problems and in particular the switchbetween HAM and EGGS worked properly and rapidly.1. IntroductionThe ground–based spectroscopic monitoring of the CoRoT tar-gets continued in June and July 2011. Two sites have beeninvolved: European Southern Observatory (La Silla, Chile;HARPS@3.6m) and Observatoire de Haute Provence (France;SOPHIE@1.9m).The next HARPS runs are scheduled from December 17,2011 to 27, 2011 and from January 7 to 12, 2012. ThierryMorel (Liege University) and Monica Rainer (Brera Observa-tory) will be the observers. No other observations with otherinstruments are scheduled, the OHP proposal has not beenaccepted. We will evaluate the possibility to take complemen-tary spectra from the MERCATOR telescope (HERMES in-strument; Canary Islands).2. Status of publicationsTable 1 lists the status of the analyses of the spectroscopictimeseries, and the new attributions as well. New entries withrespect to the previous report are highlighted in red. Afterpublication of the results in a refereed journal, the reducedspectra have been made available to the community throughthe ESO archive (ESO rule for Large Programmes).The current policy about co-autorship is to include thePIs of the Large Programmes (i.e., P. Amado, P. Mathias,E. Poretti), the observers of the specific star and, if the ESOdata are used, M. Rainer, who reduced the ESO spectra forthe whole team. The contribution of other instruments (HER-CULES, FIES, HERMES, NARVAL, FRESCO,...) should beevaluated case by case. Moreover, in the second round of pa-pers at least one of the scientists in the ground-based activitieswill be included in the first positions, to reward the great andlong effort made to support CoRoT photometry with high-resolution spectroscopy.3. The spectroscopic data of stars observed in Juneand July 2011The CoRoT observations ran from April 5 to June 30 (LRc07)and from July 6 to early October 2011 (LRc08) in the Centerdirection. The asteroseismic targets were the same for bothruns, i.e., HD 170053 (K2 III, V=7.3), HD 170031 (K5, V=8.2),HD 170231 (K2, V=8.7), HD 170174 (K2, V=8.3), and HD170200 (B8, V=5.7). All these stars are in the field of the opencluster NGC 6633.The fact that four stars out of five are red giants (HD170053, HD 170031, HD 170231, and HD 170174) imposed achange in the observational strategy with respect to previousruns. The sharp lines of these slow rotators are more suitablefor the study of the radial velocity variations than of the lineprofile ones. Therefore, we used HARPS in the HAM (high res-olution) configuration, instead of the EGGS (high efficiency)one. The corresponding increase in the exposure times imposeda limit to the number of targets. After a quick look to theCoRoT N0 photometric data (courtesy from Reza Samadi),2we omitted the less promising target HD 170174 from the con-tinuous monitoring.We had the same problems in the observations scheduledat OHP. We agreed with P. Mathias to observe HD 170031and HD 170053 in the high–resolution mode with SOPHIE,since otherwise the OHP time series would be dense enough.We observed HD 170031 and HD 170053 from both sites andwe could obtain accurate radial velocity curves. The end ofnight in OHP coincided with the beginning of night in La Sillaand the telescopes could point to the same star for 45 minutes.This allowed us to calculate the exact amount of the system-atic difference (a few m s−1) between the two spectrographsand consequently to improve the quality of the radial-velocitycurves.A few other CoRoT targets were observed at ESO. Theyare HD 172046 (upon request from P. De Cat), HD 169392AB(from R. Garcia), and HD 169556 (from G. Verner).3.1. Saving the log of the night and the RV measurementsAt the end of night it is possible to save two log-files, i.e.,the log of all spectra (spectra harps) and the list of the radialvelocities measured by the pipeline (rv harps).To do it, digitcd /diska/home/harusrin the pipeline computer (whaldrs2). It is advisable to createa subdirectory with your name:mkdir yournamecd yournamethen digit the two commands:list spectra harps yyyy-mm-dd > yyyy-mm-dd log.vdblist rv harps yyyy-mm-dd > yyyy.mm.dd rv.vdbAfter that, you can ftp the two text files everywhere youlike. If you want to see the data of your targets, both raw andreduced, first open a window in the whaldrs2 computer. Todo that, in the screen of the HARPS pipeline click with theleft button of the mouse outside any window: a small windowwill then appear; click with the left button of the mouse onharusr on whaldrs2 and the window of the desired computerwill appear. The raw and reduced spectra are in/data/raw/yyyy-mm--dd/data/reduced/yyyy-mm-dd3.2. The HAM observing blocksAn example of observing block requiring the HAM mode isreported in the Appendix. The Thorium lamp must be puton the second fiber. As in the case of the observation of coldstars in the EGGS mode, Observers are requested to carefullycheck the value of the TEL.TARGET.RADVEL keyword. It mustbe “−99999”. In such a case the HARPS pipeline calculates avery accurate value of the star’s radial velocity. Still better, itis recommened to substitute the “−99999” value with the valuecalculated by the pipeline from the first spectra of the star. Weremind that for stars with spectral type earlier than F0, thereis no template in the HARPS library and the RV value is notreliable. Often the pipeline crashes. In such a case, but onlyfor hot stars, put “99999” in the TEL.TARGET.RADVEL keyword.See also the report of the third run of the LP 182.D-0356.3.3. Observing cycleExposure times have been set to 450 sec for HD 170053(V=7.3), to 900 sec for HD 170031 (V=8.2), and to 1200 secfor HD 170231 (V=8.7). We achived the goal to get errors notlarger than 1 m sec−1 (i.e., SNR=150 at 600 nm) on the ra-dial velocity values. To study the line profile variations of HD170200 (V=5.7) the exposure time was set to 300 sec to getSNR=200 in the blue. All the spectra of these stars were takenin the HAM mode. The exposure times were often modified ac-cordingly to the weather conditions (clouds, poor seeing, ...).The red giants HD 170053, HD 170031, and HD 170231were observed in sequence and the observers tried to allocatethree spectra per night of HD 170200. As a result, we got 10-11cycles of the three red giants per night. The other CoRoT tar-gets HD 172046, HD 169566, and HD 169392AB were observedin EGGS mode. This implies that for the first time the ob-servers switched from EGGS to HAM modes during the night.The procedure took 1-2 minutes and worked fine all times butone (15 min lost). As a result, the observers performed 10-11cycles of the three red giants per (good) night and also com-pleted the survey of other targets as requested.The calibration star HD 135240 was observed at the be-ginning of the night both in HAM end EGGS mode to betterdefine the blaze function (HAM exposure time: 300 sec).3.4. Length of the nightsThe observations spanned about 12h in June and about 11h30min July. At the declination of the CoRoT field (from +6◦to −3◦), the HARPS observations could be performed from−4h20m to +4h20m. At these extreme hour angles the airmassis 2.8, i.e., the critical telescope pointing limit. In the case ofthe LRc07 pointing (+6◦), the CoRoT field could be observedfor about 8h in both runs.3.5. Weather statisticsThe observations in the 10-nights run were exceptionally goodfor the month of June. In the first run we lost 12.25 hours (outof 120) due to bad weather (11.25 hours during the visibilityof the CoRoT targets, 1.0 hour during the filling programme).In the second run we lost three full nights i.e., 34.5 hours(out of 57.5) due to bad weather (24 hours during the visi-bility of the CoRoT targets, 10.5 hours during the filling pro-grammes).4. Backup and filling programmesOther targets have been observed at the beginning and at theend of nights (filling programme), strictly following the ESOrules in the submission of these additional targets. We remindthat both backup and filling programmes have to be submittedby the PI 10 days before the observations and then approved bythe ESO staff. The stars belonging to other accepted proposalsare rejected. This occurred for several stars of the backup andfilling programmes proposed for the June-July runs.In addition to HR 6139 (P.I. L. Mantegazza, 5 spectra on 3nights) and HD 91024 (P.I. C. Aerts, 19 spectra on 9 nights),we observed:γ Dor and SPB stars (P.I. P. De Cat) – HD 163899 (1 spec-trum), HD 91201 (1), HD 73654 (1), HD 112409 (1), HD 155854(1), HD 224288 (1), HD 138521 (1), HD 133803 (1), HD 856933Table 1. Targets observed in the framework of the ESO ground–based complementary observations. New entries are in red.The responsibles of the analysis of the spectroscopic data are also listed.Star CoRoT run – ESO LP Investigators PapersSpectroscopic dataPublished resultsHD 49434 LRa01 - LP 178.D-0361 Uytterhoeven et al. 2008, A&A, 489, 1213HD 50747, HD 51106 IR01 - LP 178.D-0361 Dolez et al. 2009, A&A, 506, 159HD 50844 IR01 - LP 178.D-0361 Poretti et al. 2009, A&A, 506, 85HD 50846 IR01 - LP 178.D-0361 Desmet et al. 2010, MNRAS, 401, 418HD 181231 LRc01 - LP 178.D-0361 Neiner et al. 2009, A&A, 506, 143HD 180642 LRc01 - LP 178.D-0361 Briquet et al. 2009, A&A, 506, 269HD 50209 LRa01 - LP 178.D-0361 Diago et al. 2009, A&A, 506, 125HD 49330 LRa01 - LP 178.D-0361 Floquet et al. 2009, A&A, 506, 103HD 46149 SRa02 - LP 182.D-0356 Degroote et al. 2010, A&A, 519, A38HD 49434 - Paper II LRa01 - LP 178.D-0361 Chapellier et al. 2010, A&A, 2011, 525, A23HD 51756 LRa02 - LP182.D-0356 Papics et al., 2011, A&A, 528, A123CoRoT 101155310 LRc01 - LP 182.D-0356 Poretti et al. 2011, A&A, 528, A147Papers in preparationHD 181555 LRc01 - LP 178.D-0361 L. Mantegazza Michel et al.HD 171586 LRc02 - LP 178.D-0361 T. Luftinger Luftinger et al.HD 172189 - Paper III LRc02 - LP 178.D-0361 S. Mart́ın Mart́ın et al.HD 50870 LRa02 - LP 182.D-0356, LP 185.D-0056 L. Mantegazza Mantegazza et al.HD 51193 LRa02 - LP 182.D-0356 J. Gutierrez-SotoHD 174966 SRc01 - LP 182.D-0356 L. Mantegazza Garcia-Hernandez et al.HD 50230 LRa01 - LP 182.D-0356 P. Degroote Degroote et al.Analyses in progress - Line profile variationsHD 49434 - Paper III LRa01 - LP 178.D-0361 K. Uytterhoeven Uytterhoeven et al.HD 171834 LRc02 - LP 178.D-0361, LP 182.D-0356 K. UytterhoevenHD 51452 LRa02 - LP 182.D-0356 M. FloquetHD 174532 SRc02 - LP 182.D-0356 L. Mantegazza Fox et al.HD 170580 LRc05 - LP 182.D-0356, LP185.D-0056 A. ThoulHD 44195 LRa03 - LP 182.D-0356 E. Poretti Poretti et al.HD 43317 LRa03, LRa02 - LP 182.D-0356 P. PapicsHD 170699 LRc05, LRc06 - LP 185.D-0056 L. MantegazzaHD 170973 LRc05, LRc06 - LP 185.D-0056 Th. LuftingerHD 170783 LRc05, LRc06 - LP 185.D-0056 M. BriquetHD 171219 LRc05 - LP 185.D-0056 C. NeinerHD 41641 LRa05 - LP 185.D-0056 L. MantegazzaHD 43285 LRa04 - LP 185.D-0056 C. NeinerHD 43338 LRa04 - LP 185.D-0056 Ph. MathiasHD 42597 LRa05 - LP 185.D-0056 P. DegrooteHD 170031, HD 170231 LRc07, LRc08 - LP 185.D-0056 T. Morel, E. Poretti (RV)HD170053 LRc07, LRc08 - LP 185.D-0056 T. Morel, E. Poretti (RV)HD 170200 LRc07, LRc08 - LP 185.D-0056 P. DegrooteAnalyses in progress - Binarity and/or physical parametersHD 51844, HD 49310 LRa02, SRa01 - LP 182.D-0356 M. HareterRed giants All LPs, not still observed by CoRoT T. MorelGSC00144-03031 LRa04 - LP 185.D-0056 E. Poretti Poretti et al.HD 50890 IRa01 - LP 185.D-0056 Th. Morel Barban et al.HD 49566 SRa01 - LP 185.D-0056 Th. Morel Hekker et al.HD 43587 LRa03 - LP 185.D-0056 P. Boumier Boumier et al.HD 42299 LRa04 - LP 185.D-0056HD 42787 LRa04 - LP 185.D-0056 H. BrunttHD 42089 LRa05 - LP 185.D-0056 H. BrunttHD 42618 LRa04, LRa05 - LP 185.D-0056 M. Hall I. Roxburgh et al.HD 170174 LRc07, LRc08 - LP 185.D-0056 T. MorelHD 172046 LRc02 - LP 185.D-0056 P. De CatHD 169392AB LRc03 - LP 185.D-0056 H. Bruntt Garcia et al.HD 169556 LRc03 - LP 185.D-0056 H. Bruntt Verner et al.4Table 3. General description of the nightsSeeing Lost time NotesNight DIMM Bad weather Technical ReasonsJune 23-24 0.′′5–1.′′0June 24-25 0.′′5–1.′′2June 25-26 0.′′7–1.′′5 Thin cloudsJune 26-27 0.′′5–1.′′5June 27-28 ∼1.′′2 Simultaneous observations with OHPJune 28-29 < 0.′′8June 29-30 0.′′4–0.′′8 15min EGGS-HAM switchJune 30-July 1 ∼0.′′9 5h30min Clouds first part of nightJuly 1-2 ∼1.′′0July 2-3 1.′′5–2.′′5 6h45min Strong windJuly 15-16 12h30min Wind, rainJuly 16-17 12h30min Snow, iceJuly 17-18 2.′′0July 18-19 12h30min CloudsJuly 19-20 1.′′0 20min Pipeline stallTable 2. Number of spectra collected in the OHP and ESOruns from May to July 2011ESO observations LRc07 and LRc0810-n run 5-n run TotalHD 170031 92 19 111HD 170231 81 19 100HD 170053 84 18 102HD 170174 1 – 1HD 170200 26 5 31ESO observations other runsHD 172046 4 1 1HD 169392A 1 – 1HD 169392B 1 – 1HD 169556 – 1 1OHP observationsHD 170031 76HD 170053 175(1), HD 90872 (1), HD 113357 (1), HD 79416 (1), HD 149989(1), HD 110606 (1), HD 126516 (1), HD 152565 (1), HD 86659(1), and HD 188032 (2 spectra).B-A-F stars (P.I. M. Hareter) – EE Cha (2 spectra), EF Cha(2), HD 144277 (4), υ Sco (3), µ1 Sco (3), ζ1 Sco (3). Moreover,13 additional spectra of HD 144277 were taken on the nightJuly 2-3, when the strong wind hampered the pointing in thedirection of the CoRoT field.δ Sct stars (P.I. E. Poretti) - Gravity darkening effect: 35 spec-tra of WZ Scl and 38 spectra of ρ Pav at end of 9 nights ofthe first run (all except the first). v sin i determinations: 1spectrum of 32 stars at end of two nights of the second run.5. AppendixHere we list the Observing Block of HD 170031 as saved fromthe P2PP software. The HAM configuration with the sci-ence fiber only is defined by the ACQUISITION.TEMPLATE.NAMEkeyword. Consecutive exposures can be taken changing theSEQ.NEXPO keyword. For other objects, the lines name, ra,dec, TARGET.NAME, DET1.WIN1.UIT1 must be changed. Notethat the exposure time is in the DET1.WIN1.UIT1 keyword.IMPEX.VERSION "2.0"type "O"STTimeIntervals ""calibrationReq ""InstrumentComments ""userComments "HD170031 K5 V=8.19"userPriority "1"LineNumber "0"name "A0-HD170031-HAM"comments ""objectClass " Unknown "ra " 18:27:07.390"dec " 06:04:11.413"epoch "2000.0"equinox "2000"propDec "0.000000"propRA "0.000000"diffRA "0.000000"diffDec "0.000000"LineNumber "0"TARGET.NAME "HD170031"air_mass "5.0"fractional_lunar_illumination "1.0"5sky_transparency "Photometric"moon_angular_distance "30"seeing "2.0"StrehlRatio "0.0"CONSTRAINT.SET.NAME "No Name"longDescription ""IPVersion "150.28"instrument "HARPS"LineNumber "0"OBSERVATION.DESCRIPTION.NAME "HD170031"ACQUISITION.TEMPLATE.NAME "HARPS_ech_acq_thosimult"TEL.TARG.RADVEL "-99999"INS.OPTI6.NAME "THAR2"DPR.TYPE "STAR,WAVE,K5"TEMPLATE.NAME "HARPS_ech_obs_all"DET1.READ.SPEED "416kHz,1,high"DET1.WIN1.UIT1 "900"SEQ.NEXPO "1"DPR.CATG "SCIENCE"

Report on the third run of the ESO LP 185.D-0056 (HARPS@3.6m)

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Report on the third run of the ESO LP 185.D-0056 ([email protected])

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