The ESO Large Programme 185.D-0056 started with the HARPS instrument at the 3.6m ESO telescope in June and July 2010. The log of the these observations, the problems encountered, some tips, the situation of the publications, and a look to the future are given

PORETTI, Ennio

RAINER, Monica

Suarez, Juan Carlos

Uytterhoeven, Katrien

OA@INAF - Istituto Nazionale di Astrofisica

2010Publication Year2023-02-24T08:58:41ZAcceptance in OA@INAFReport on the first run of the ESO LP 185.D-0056 (HARPS@3.6m)TitlePORETTI, Ennio; Suarez, Juan Carlos; Uytterhoeven, Katrien; RAINER, MonicaAuthorshttp://hdl.handle.net/20.500.12386/33805Handle8NumberReport on the first run of the ESO LP 185.D-0056(HARPS@3.6m)E. Poretti, J.C. Suarez, K. Uytterhoeven, and M. RainerSeismology Ground-Based Observation Working GroupAugust 31st, 2010; Version 1.0EXECUTIVE SUMMARY.The ESO Large Programme 185.D-0056 started with theHARPS instrument at the 3.6m ESO telescope in June andJuly 2010. The log of the these observations, the problemsencountered, some tips, the situation of the publications, anda look to the future are given. The following actions/items areemphasized:1. The observations in the 15 nights were disturbed by clouds,humidity, and wind. The δ Sct star HD 170699, the Be starHD 171219, the β Cep HD 170580 were observed to studyline profile variations. Spectra were also obtained for theB-star HD 170783 and for the CP star HD 170973. Allthese stars are belonging to the LRc05 and LRc06 CoRoTpointings. Moreover, we observed the bright red giant HR7349 (LRc01).2. Different filling programmes were run at the beginning andend of night. They were also used as backup programmeswhen strong wind from North hampered the pointing ofthe CoRoT field.3. For the first time we had serious technical problems.HARPS did not work properly in the the EGGS config-uration and we were forced to observe in the HAM config-uration in one full night. Moreover, another full night waslost due to guiding problems.1. IntroductionThe ground–based spectroscopic monitoring of the CoRoT tar-gets continued in June and July 2010. Two sites have beeninvolved: European Southern Observatory (La Silla, Chile;HARPS@3.6m) and Observatoire de Haute Provence (France;SOPHIE@1.9m). As in the previous cases, the goals of thiseigth (the fourth of the HARPS series) internal report are tocirculate useful information about the ESO observations withinthe team and to keep the record of the observations.The next HARPS runs are scheduled from December 22,2010 to January 1, 2011 and from January 7 to 12, 2011. Inter-ested observers are kindly requested to inform E. Poretti. Notethat the two runs are separated by 6 days only and thereforethe observations could be conducted by just one observer. Insuch a case, we will ask ESO to give full support to the observerfor the whole period. In Period 86 HARPS will be offered inthe polarimetric mode too. We submitted a request (a shortproposal) to the OPC to use the instrument in such mode. Wehave been informed that “ the OPC judged that the intendedpolarimetric observations represent too large a deviation fromthe original goals and observational strategy of the Large Pro-gramme to allow them to be approved on the basis of a merechange request. The OPC recommended that, in future periods,you request additional time for such observations via full for-mal proposals to be submitted by the corresponding deadlines”.To complement the HARPS observations of the nextCoRoT pointing there will be a SOPHIE@ OHP run from De-cember 10 to 20 (P.I.: P. Mathias). We will evaluate the pos-sibility to take complementary spectra from the MERCATORtelescope (HERMES instrument; Canary Islands).2. Status of publicationsTable 1 lists the status of the analyses of the spectroscopictimeseries, and the new attributions as well. After publica-tion of the results in a refereed journal, the reduced spectrahave been made available to the community through the ESOarchive (ESO rule for Large Programmes). New papers withrespect to the previous report are highlighted in red.I suggest that in the second round of papers at least one ofthe scientists in the ground-based activities will be included inthe first positions, to reward the great and long effort made tosupport CoRoT photometry with high-resolution spectroscopy.3. The spectroscopic data of stars observed in Juneand July 2010The CoRoT observations performed by CoRoT from April toSeptember 2010 in the Center direction were splitted into twoLong Runs (LRc05 and LRc06), each spanning 80 days. The as-teroseismic targets are: HD 170699 (δ Sct, V=7.0), HD 1705802(β Cep, V=6.7), HD 170973 (CP star, V=6.4), HD 170783 (Bstar, V=7.7), and HD 171219 (Be star, V=7.6).The Red Giant HD 171264 (V=8.1) was too faint and notvery appealing. We replaced it with the bright Red Giant HR7349≡HD 181907 (V=5.8) observed by CoRoT in the LRc01(Carrier et al. 2010, A&A 509, A73).These stars were also observed with SOPHIE@OHP (June21-28, 2010) and HERMES@Mercator.4. The ESO observationsThe observers were Juan Carlos Suarez (IAA, 12-22 June,2010) and Katrien Uytterhoeven (CEA, 1-6 July, 2010). Ta-bles 2 and 3 report the logs of both runs. The setup of theHARPS instrument is summarized in the Appendix of the pre-vious report. We just remind that the instrument must be setin the EGGS mode (i.e., lower resolution mode), correspond-ing to R=80,000, as measured on the spectra we obtained.We definitely solved the instrumental problem affecting theHARPS spectra collected in 2009. The corrected spectra weredistributed to the respective PIs (see Tab. 1) in March.Observers are requested to carefully check the value of theTEL.TARGET.RADVEL keyword in the Observing Blocks. It mustbe “–99999.9” or “–99999” for the cold stars. In such a case theHARPS pipeline calculates a very accurate value of the star’sradial velocity. For stars with spectral type earlier than F0,there is no template in the HARPS library and the RV value isnot reliable. 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-0356.4.1. Observing cycleExposure times have been set to 700 sec for HD 170699, to400 sec for HD 170973, to 500 sec for HD 170580, 210 sec forHR 7349, and to 1200 sec for HD 171219. However, these ex-posure times were often modified accordingly to the weatherconditions (clouds, poor seeing, ...). The observing sequencewasHR 7349 - HD 170699 - HD 171219 - HD 170699 - slot - ...In the “slot” we put HD 170973 at the beginning and end ofnight and, in alternance, HD 170580 and HD 170783 duringthe night.HD 135240 was observed at the beginning of the night tobetter define the blaze function (exposure time: 150 sec).4.2. Length of the nightsThe observations spanned about 12h30m in June and about11h30m in July. At the declination of the CoRoT field (from+6◦ to −3◦), the HARPS observations could be performedfrom −4h20m to +4h20m. At these extreme hour angles theairmass is 2.8, i.e., the critical telescope pointing limit. TheCoRoT field could be observed for about 9h in both runs.The night of 23-24 June started at UT 22h25m≡ST 11h51mand ended at UT 10h56m≡ST 24h23m. The night of 1-2 July started at UT 23h03m≡ST 12h59m and ended atUT 10h32m≡ST 24h30m.4.3. Weather statisticsThe observations were often disturbed by clouds, humidity, andstrong wind. In the first run we lost 33.5 hours (out of 125) dueto bad weather (26.5 hours during the visibility of the CoRoTtargets, 7.0 hours during the filling programme). In particular,two full nights were lost (15-16 and 18-19 June). Moreover, 2hand 9h of the CoRoT time could not be used due to strongwind from North on the 12-13 and 17-18 June, respectively.In the second run we lost 20.5 hours (out of 57.5) due to badweather (16 hours during the visibility of the CoRoT targets,4.5 hours during the filling programme). Moreover, 5h and 1hof the CoRoT time could not be used due to strong wind fromNorth on the nights of 4-5 and 5-6 July, respectively.4.4. Technical reasonsFor the first time we had to face severe technical problems.They were of different nature (a slight drift in the EGGSfiber, problems in closing the EGGS shutter and in the cal-ibration procedure). In the first run we lost 20 hours, 9 duringthe CoRoT time, 11 of the filling programme. We used theHAM configuration in one full night (14-15 June) to bypassthe EGGS malfunction. The step in wavelength of the HAMspectra has been made the same of the EGGS ones. We lost 1full night for the guiding problems (19-20 June), common toboth HAM and EGGS configurations.After some maintenance and repair procedures, the ESOstaff solved the problem and in the second run we lost 15m inthe twilight of the night of 1-2 July only.4.5. Overall statisticsIn the first run we lost 53.5 hours due to bad weather andtechnical problems. The CoRoT field was monitored for 43.5hours, the filler and backup stars for 28.0 hours (11 hours ofthe CoRoT time had to be given to the backup programmedue to the wind from North).In the second run we lost 20.5 hours due to bad weatherand technical problems. The CoRoT field was monitored for24.0 hours, the filler and backup stars for 13.0 hours (7 hoursof the CoRoT time had to be given to the backup programmedue to the wind from North).We had a bonus of 4h40m in the extra-night of June 30-July1 (3h50m for the CoRoT field, 50m for the filler programme).4.6. Signal–to–noise ratio evaluationThe SNRs listed in Table 3 are the median values of the SNRsin the region 5802–5825 Å. They have been computed duringour reduction taking into account photon noise, readout noiseand flat field correction. We confirm that the values providedby the HARPS pipeline at the telescope are in general overes-timated by a factor of 1.25.5. Backup and filling programmesThe strong wind blowing from the North forced the observersto move to the backup programme during 4 (partial) nights (17-18 and 12-13 June, 4-5 and 5-6 July). The backup programmewas composed of a list of γ Dor, SPB, Be stars to be observedonce.Other targets have been observed at the beginning andat the end of nights (filling programme), strictly following the3Table 1. Targets observed in the framework of the ESO ground–based complementary observations. The responsibles of theanalysis of the spectroscopic data are also listed.Star CoRoT run - ESO LP Investigators PapersSpectroscopic dataPublished results∗HD 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, in pressHD 49434 - Paper II LRa01 - LP 178.D-0361 Chapellier et al. 2010, acceptedPapers 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.Analyses in progressHD 49434 - Paper III LRa01 - LP 178.D-0361 K. Uytterhoeven Uytterhoeven et al.HD 172189 - Paper III LRc02 - LP 178.D-0361 S. Mart́ın Mart́ın et al.HD 171834 LRc02 - LP 178.D-0361, LP 182.D-0356 K. UytterhoevenHD 50870 LRa02 - LP 182.D-0356 L. Mantegazza Mantegazza et al.HD 51452 LRa02 - LP 182.D-0356 M. FloquetHD 51193 LRa02 - LP 182.D-0356 J. Gutierrez-SotoHD 174966 SRc01 - LP 182.D-0356 L. Mantegazza Garcia-Hernandez et al.HD 174532 SRc02 - LP 182.D-0356 L. MantegazzaHD 170580 LRc05 - LP 182.D-0356, LP185.D-0056 C. AertsHD 44195 LRa03 - LP 182.D-0356 E. PorettiHD 43317, HD 51756 LRa03, LRa02 - LP 182.D-0356 P. PapicsHD 51844, HD 49310 LRa02, SRa01 - LP 182.D-0356 M. HareterRed giants All LPs, not still observed by CoRoT T. MorelHR 7349 LRc01 - LP185.D-0056 F. CarrierHD 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 C. AertsHD 171219 LRc05 - LP 185.D-0056 C. Neiner∗ Reduced spectra now available in the ESO archive athttp://archive.eso.org/cms/eso-data/data-packages/178-d-0361/hd-49434-feros-spectroscopic-time-series-data-release-v1-0/http://archive.eso.org/cms/eso-data/data-packages/178-d-0361/hd-50844-feros-spectroscopic-time-series-data-release-v1-0/http://archive.eso.org/cms/eso-data/data-packages/178-d-0361/hd-49330-feros-spectroscopic-time-series-data-release-v1-0/http://archive.eso.org/cms/eso-data/data-packages/178-d-0361/hd-51106-hd-50747-feros-spectroscopic-time-series-data-release-v1-0/http://archive.eso.org/cms/eso-data/data-packages/178-d-0361/hd-180642-feros-spectroscopic-time-series-data-release-v1-0/http://archive.eso.org/cms/eso-data/data-packages/178-d-0361/hd-181231-feros-spectroscopic-time-series-data-release-v1-0/http://archive.eso.org/cms/eso-data/data-packages/178-d-0361/hd-50209-feros-spectroscopic-time-series-data-release-v1-0/ESO rules in the submission of these additional targets. In ad-dition to ε Lup (P.I. K. Uytterhoeven, 9 spectra, SNR between170 and 335), HD 137949 (P.I. F. Leone, 10 spectra, SNR 110-250), HD 91024 (P.I. C. Aerts, 16 spectra, SNR 110-260), weobserved:Be stars (P.I. A.M. Hubert) – 1 spectrum of Mis 379, Mis 270,MQ TrA, µ Lup, HD 146596, V846 Ara, µ Cen, HD 156398, HD146501 (SNR=120), θ Cir, V946 Cen, HD 151113, HD 147302,HD 155851, V817 Cen, µ2 Cru, HD 124834, CO Cir, γ Cir,CK Cir, HD 216113 (SNR=90). SNR values are in the range165-230, if not differently noted. Two spectra of CV Cir (SNR120 and 200).γ Dor and SPB stars (P.I. P. De Cat) – HD 112409 (2 spectra),HD 85693 (2), HD 110606 (2), HD 90872 (2), HD 138521 (1,SNR=105), HD 152635 (2), HD 197451 (1 EGGS; 2 HAM,SNR 70 and 140), HD 201985 (1 EGGS, SNR=85; 1 HAM,SNR=65), HD 224288 (1), HD 206481 (2, SNR 110 and 175),HD 214291 (6), HD 205879 (1), HD 10167 (1), HD 11462 (1),HD 109799 (1), HD 113357 (2), HD 152565 (2), HD 155854 (1),HD 121190 (1), HD 131058 (1), HD 132200 (1), HD 137785 (1),4Table 2. General description of the nightsSeeing Lost time NotesNight DIMM Bad weather Technical ReasonsJune 12-13 1.′′9–2.′′6 2h15min 1h15min EGGS fiber lost. Clouds, strong wind.June 13-14 1.′′8–2.′′0 6h20min 2h Dome control. Clouds.June 14-15 <1.′′5 3h30min EGGS shutter, observations in HAM mode.June 15-16 12h30min Clouds all the night.June 16-17 1.′′2 45min EGGS calibration problem.June 17-18 1.′′4–1.′′8 Strong wind from North, backup programme.June 18-19 12h30min Fog, high humidity (100%).June 19-20 12h30min Guiding problems, both HAM and EGGS.June 20-21 1.′′0 No problems.June 21-22 1.′′3–1.′′9 Thin cirrus.June 30-July 1 0.′′85 Extra half-nightJuly 1-2 0.′′5–0.′′9 15min Telescope control stuck. Seeing 1.′′0–1.′′2 end-of-nightJuly 2-3 1.′′3–2.′′4 1h10min Strong wind.July 3-4 2.′′0–3.′′0 9h45min Strong wind.July 4-5 >2.′′0 4h15min Strong wind.July 5-6 >2.′′0 5h15min Strong wind (4.′′5 end-of-night), backup programme.HD 149989 (1), HD 153580 (1), HD 79416 (2), HD 84809 (1),HD 86659 (1). SNR values are in the range 130-240, if notdifferently noted.A-F stars (P.I. M. Hareter) – HD 114839 (2 spectra, SNR 105and 185), HD 209775 (2, SNR 125 and 190), BD+18◦4914 (1spectrum, SNR=80).CARMENES scientific case (P.I. P. Amado) – The M-dwarfstar Gl 570B has been monitored on two nights in the frame-work of the preparation of the scientific case of the spectro-graph CARMENES, which will be mounted at the 2.2m tele-scope of Calar Alto. Gl 570B has been monitored for 2 hours(46 spectra, Texp=120 sec, SNR from 27 to 53) in the night of12-13 June and for 85 min (52 spectra, Texp=60 sec, SNR from50 to 60) in the night of 2-3 July. Notice that in the secondnight we got the same SNR of the first one with half exposuretime. Indeed, the first night was very windy, with a poor seeing(about 2′′), while the beginning of the second night was quitegood (seeing around 1.′′3; see Table 2).We remind that both backup and filling programmes haveto be submitted by the PI 10 days before the observations andthen approved by the ESO staff. The stars belonging to otheraccepted proposals are rejected. This occurred for several starsof the backup and filling programmes proposed for the June-July runs.5Table 3. Log of the observing runs (June 2010–July 2010) at ESO with the HARPS@3.6m instrument. The number of spectraand the measured SNR range are indicated for every star on each night. Spectra with low SNR have not been counted.Night HD 170699 HD 170580 HD 170973 HD 170783 HD 171219 HR 7349V=7.0 V=6.7 V=6.4 V=7.7 V=7.6 V=5.8Exp. Time 700 sec 500 sec 400 sec 1100 sec 1200 sec 210 sec(Default)June 12-13 8 2 – 1 – 4[123-190] [135-220] [107] [150-230]June 13-14 3 – 1 – 2 1[120-152] [145] [125-141] [133]June 14-15 11 1 1 2 6 6(HAM spectra) [104-204] [180] [97] [130-154] [109-198] [123-191]June 15-16 – – – – – –June 16-17 15 2 1 2 7 7[113-233] [182-230] [202] [164-201] [143-223] [193-288]June 17-18 6 1 1 – 3 2[172-225] [202] [185] [161-182] [212-222]June 18-19 – – – – – –June 19-20 – – 2 – – –[58-67]June 20-21 12 3 1 2 6 10[103-173] [120-152] [160] [121-140] [97-166] [109-206]June 21-22 11 2 2 2 5 7[110-181] [136-153] [83-150] [155-168] [105-177] [104-187]Jun 30-Jul 1 6 1 1 – 2 19[204-240] [184] [220] [198-226] [152-245]July 1-2 22 5 2 4 11 22[176-230] [165-220] [218-237] [203-257] [165-235] [199-282]July 2-3 15 2 2 2 7 14[137-228] [255-255] [190-255] [195-203] [144-227] [193-294]July 3-4 1 – – – – 8[112] [180-243]July 4-5 – 1 – – – 6[97] [164-212]July 5-6 – 2 2 – – 10[154-185] [123-168] [106-245]Total ESO 110 22 16 15 49 116Total OHP 31 15 10 – 13 –

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

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

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