Accurate Characterization of Transiting Extrasolar Planets

Time Allocation Committee for Application No. MPG time at the ESO 2.2m-telescope c/o MPI f¨urAstronomie Observing period P93 K¨onigstuhl17 Received D-69117 Heidelberg / Germany

APPLICATION FOR OBSERVING TIME

from X MPIA MPG institute other

1. Telescope: 2.2-m X L

2.1 Applicant Dr. Luigi Mancini Max Planck Institute for Astronomy Name Institute K¨onigstuhl 17 69117 Heidelberg street ZIP code - city mancini [email protected] ESO User Portal username e-mail

2.2 Collaborators S. Ciceri, Th. Henning MPIA name(s) institute(s)

name(s) institute(s)

2.3 Observers Luigi Mancini Simona Ciceri name name By specifying the names under item 2.3 it is obligatory to also send out these observers to La Silla, if required. Correspondence on the rating of this application will be sent to the applicant (P.I.) as quoted under 2.1 above.

3. Observing programme: Category: E

Title : Accurate characterization of transiting extrasolar planets Abstract : Our two large programs, dedicated to conﬁrm and characterize the properties of transiting extrasolar planets (TEPs) by broad-band photometry and defocussing method with the GROND imaging system at the MPG/ESO 2.2m telescope, turn out to be a great success and have so far resulted in the conﬁrmation of 3 new HATSouth TEPs and characterization of 6 known TEPs. In 3 cases we detected anomalies on the light curves which are compatible with starspots on the photosphere of the parent stars. The atmosphere of 5 TEPs was probed by studying their radius variation as a function of the wavelength. Considering the good results achieved so far, we present a new joined proposal to continue to use GROND to obtain accurate photometric follow-up transit light curves of new and known TEPs.

4. Instrument: WFI FEROS X GROND

5. Brightness range of objects to be observed: from 10.1 to 15.1 V mag

5 6. Number of hours: applied for already awarded still needed 115 285 200 no restriction grey dark

7. Optimum date range for the observations: ...... 01.04.2013 – 30.09.2014 Usable range in local sideral time LST: ...... 23:30h – 04:00h 8a. Description of the observing programme

Astrophysical context try, i.e. light curves with point-to-point scatters lower than 1.0 mmag in the optical bands and ∼ 2.0 mmag in One of the most efficient techniques to detect extraso- the near infrared ones. The achieved light curves will lar planets is the transit method, which is based on be then analyzed (i) to confirm the planetary nature the periodic shallow dip in the light curves of exo- in the case of HATSouth candidates; (ii) to obtain the planet host stars. The amount of the star dim de- radii of the transiting planets with a precision of a few pends on the relative sizes of the star and the transit- percent; (iii) to improve the parameters of the plan- ing planet. When combined with radial velocity (RV) etary system, including transit epoch, orbital period, measurements, the transit method allows to disclose inclination, semi-major axis; (iv) to study the variation the main physical parameters of planetary systems, in- of the planet radii as a function of the wavelength and cluding the temperature of the planet and the evolu- comparing them with isothermal model atmospheres tionary age of the star [1]. Systematic photometric (an example is given for the planet WASP-19 b in Fig. surveys, such as WASP [2], HAT-Net [3], TrES [4], Ke- 4). This study will therefore place several constraints pler [5], etc., have played a major role in this scientific about the composition of several hot-Jupiters atmo- process, achieving a high return in terms of planet dis- spheres. coveries (> 300). In 2009 the MPIA became one of the main partners of the first global southern network: HAT-South [6]. This network consists of six identical, Previous work fully automated wide field telescopes, located at three Simultaneous multi-band observations of different sites in the southern hemisphere. The primary pur- planetary transits with GROND have been already per- pose of the project is to detect and characterize a large formed by our group (see another example in Fig. 3), number of transiting extrasolar planets (TEPs) and to obtaining low-scattered light curves that lead to accu- explore their diversity. The three ground sites permit rate measurements of the photometric properties of the near round-the-clock monitoring of selected fields, and examined planetary systems [12, 13, 14, 15]. We also the continuous data-stream greatly enhances recovery used GROND to confirm several planetary candidates of transits. Indeed, our global network of telescopes detected by the HAT-South survey, such as HATS-1 b produces well over 100 candidates each year. Several [7], HATS-2 b [8] (Fig. 2) and HATS-3 b [9] (Fig. 3). of them have been successfully confirmed as TEPs by RV measurements with FEROS and photometric time series with GROND (Figs. 1 and 2) [7, 8, 9]. Layout of observations An interesting alternative to transmission spec- We plan to study a set of TEP systems that are suf- troscopy in probing the atmospheres of TEPs is to ficiently bright to be properly observed with the 2.2m study their transits with simultaneous photometry at telescope. The final list of TEPs will be selected consid- different wavelengths. This strategy allows the ra- ering their visibility during P93 MPIA GTO periods, dius of a TEP to be measured in multiple passbands which are still unknown. Transit times were calculated and is not affected by temporal variability, for ex- from known ephemeris. In order to reduce random and ample starspots. The aim is so to detect variations systematic sources of errors (such as flat-field errors, attributable to changes in opacity at different wave- short scale seeing variations, bad tracking, etc.), we lengths. By using BUSCA [10, 11], and GROND will use the telescope-defocussing method. Depending [12, 13, 14, 15] we have pioneered this technique, which on the magnitude of the target, we will select the “fast” is now becoming a standard technique [16, 17]. or “slow” read-out mode of GROND CCDs. Just af- A classification of hot Jupiters in two classes, pM ter the sunset, or before the sunrise of each observing and pL, was suggested depending to the incident stellar night we will collect sky flatfield frames. Bias and dark flux and the expected amount of absorbing substances, frames are also requested in order to calibrate the sci- such as gaseous titanium oxide (TiO) and vanadium entific images. oxide (VO), in their atmospheres [18]. The atmosphere of planets belonging to the pM class should be rich in Strategic importance for MPIA oxidized elements, which should cause a variation of the planetary radius by ∼ 3% between the wavelength Nowadays, the subject of the Extrasolar Planets is one ranges 350–400 nm and 500–700 nm. Such a variation of the most extensively studied fields by astronomers. is directly measurable using GROND. This program, as well as the parallel one concerning RV measurements of the HATSouth candidates with the Immediate aim FEROS spectrograph (PI S. Ciceri), is of high strategic importance for the MPIA. Thanks to the ESO/MPG We propose to observe a small set (∼ 6) of robust 2.2m Telescope and the GROND imaging system, we HATSouth candidates and another small set (∼ 6) will be able to confirm and fully characterize more of suitable known TEPs with GROND by using the and more planets, strengthening the role of the MPIA telescope-defocussing technique. The GROND instru- within the community of the planetary science. ment will allow us to achieve high precision photome-

2 8b. Figures and tables

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ò Normalised 0.985 ô ò ò àôôæ àòà æôòô òòò ôò à ò æ àôææôæô à à à æ à òà àôò à æ ò ¢ ôòò æò òò àôòàôòæ à à ò æ g filter d æ æ ò g filter òôæà ò ò ò ôæ à 0.980 ôô ò àæ ò ò òò òæ ôà òæô æààà àààò òà òò òò ôôà æ ¢ ôôæôæô òô ò ò àô ô r filter àòòôò ò æ ôæ à à ôààæ 0.980 à ô ô æ r filter æ æ ôààôààà ò àòæ ô ôàôæàô æ æ ôòàò æà ò ô æàà Normalised ôæ ôæô ô ô à i filter ôæàòæ ò ôææôà ò òòà 0.975 ô æàò òôæ ôàà àæôôæ æ æ æ æ ô æ æ ôæòôàò ¢ æ æ æô ò ô òòôà à àæô à i filter ææ ò z filter ô ôæôà æàæ òæà æ ô à ôæò ààòæàæ æ ôà 0.970 òôàòæàòôæôà ¢ ò à ô z filter 2079.15 2079.20 2079.25 0.975 ô ò BJDHTDBL-2454000 2033.50 2033.55 2033.60 Figure 1: Combined four-colour transit light curves BJDHTDBL-2455000 of HATS-2 of two diﬀerent transit events observed Figure 3: Combined four-colour transit light curves of with GROND. Top panel: the bump observed just WASP-19 obtained with GROND. The bump observed after the midtransit in the transit #1 is interpreted near the centre of the transit is due to the occultation as the covering of a “cold” starspot by the planet. of a starspot by the planet [14]. Lower panel: in addition to the bump occurred near the egress part of the light curve of the transit #2, a “hot” spot manifested in the g0 band, just before the starting of the covering of the starspot [8].

1.005

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Flux àà ô æ 0.995 æ æ ò 0.146 H2O à H2O òàô Na æ ôæ à ô æ ò àò æà ô àà òæ æ ô ô ô à K òà à àô à H O òææò à ô æ 2 á Normalised à ô ôòà ô à æ 0.144 ì æ 0.990 ææ à æ H O à à à à à à ôà à ìà 2 á àà à à òæ æ æ æ æ ôæà æ à æ æ æàòæ ô æ ô ò æô à à àô àôà ææ ò ôæ ô æ ôô ô á æ òæ æ ô ô æ ôà à ô àò æ ôæ ôò ôòôò ì à ì ò ò ò òôæ ô æôææ òôò ì ôàæô æ æà òæ æ ææ ô ô æ ô ¢ á á

ò ò æ ò ò A ò ò ò ò ò ô g filter ì ì ò ò òò ¢ 0.142 á á ò ò æ r filter R à ò òò ¢ 0.985 ò à i filter b ì à ô z¢ filter R 0.140 2166.50 2166.55 2166.60 2166.65 2166.70 2166.75 BJDHTDBL-2455000 0.138 Figure 2: Combined four-colour transit light curves of HATS-3 obtained with GROND [9]. g¢ r¢ i¢ z¢ J H K 0.136 500 1000 1500 2000 wavelength HnmL Figure 4: Variation of WASP-19b’s planetary radius with wavelength. Black points are from GROND, the other coloured points are from literature. Red open boxes indicate the predicted values for the model integrated over the passbands of the observations. Transmission curves of the GROND ﬁlters are shown at the bottom of each panel. Prominent absorption features are labelled [14].

3 8e. Current logistics of PhD thesis/long term programme

This proposal is linked to the PhD thesis of Simona later than the ephemeris estimated by the sur- Ciceri. Her PhD thesis “Characterzation of Extraso- vey. It was observed again on 12.12.2012 and this lar Planets” is indeed focused on the confirmation and time the transit was fully recovered. HATS549- characterization of planetary transits. She started her 003 was recognized as a planet and renamed as Ph.D. at the MPIA in July 2012 and already performed HATS-5 (in prep.). observations of planetary transits with the MPG/ESO 2.2-m, CAHA 2.2-m, CAHA 1.23-m, Danish 1.5-m and • A partial transit of HATS580-001 b was observed Cassini 1.5-m telescopes. She is able to reduced and on 11.10.2012. The RV data for this target are analyze photometric data and is now in and advanced quite messy, probably due to the faintness of the phase in learning how to analyse stellar spectra in order parent star. The transit shape looks quite planet- to characterize stars and measure their radial velocity. like, but more RV measurements are need to se- Starting from March 2013, she has been involved in cure the orbit. the HATSouth project. The data collected through • HATS582-012 was observed on 17.10.2012. The this program will be vital for her thesis. transit was successfully recovered. The nature of the candidate should be planetary, but analysis Current status of the “HATSouth” long- is still in progress. term plan • HATS550-016 was observed on 08.12.2012. Very Part of proposed programme is based on the exploita- interesting, the joined analysis of the RV and tion of HATSouth transit data and aims in a long term photometry revealed that this a F-M eclipsing- to confirm and characterize the physical properties of binary system with the companion having a mass HATSouth exoplanets. The HATSouth survey pro- of 0.11M [21]. duces huge amount of transit candidates and period- ically releases a significant fraction of it for follow-up • HATS582-006 was observed on 11.06.2013, The studies. During P89, P90, P91, P92 periods, we al- transit was successfully recovered. The nature of ready collected photometric data of several HATSouth the candidate should be planetary, but the anal- candidates with GROND. Here we summarize the main ysis is still in progress. results that we achieved: • HATS582-004 was observed on 12.06.2013 and • HATS563-036 was observed on 21.01.2012. The 27.07.2013. The transit was successfully recov- transit was successfully recovered and the candi- ered, but both the events were affected by clouds date was recognized as a planet and renamed as resulting in incomplete light curves. The nature HATS-1 [7]. of the candidate should be planetary, but the analysis is still in progress. • HATS564-004 was observed on 28.08.2012 and 01.06.2012. The transit was successfully recov- Current status of the “accurate proper- ered in both the observations and the candi- ties of extrasolar planets” long-term plan date was recognized as a planet and renamed as HATS-2. Clear anomalies, due to the stellar We are undertaking a project aimed at characterising spots, were detected too [8]. TEPs visible from the Southern hemisphere, by obtaining high-precision light curves of their transits. We use • HATS564-007 was observed on 09.04.2012. An the telescope defocussing technique to collect photo- eclipse was detected but the candidate was re- metric measurements with very low levels of Poisson jected as an eclipsing binary. and correlated noise. Using this method at the 2.2m • HATS515-001 was observed on 07.06.2012. The telescope, we achieved light curves of remarkable precision. So far we have monitored and characterized light curve is consistent with a 1 RJup grazing transiting planet. The analysis is in progress. seven planets with GROND: GJ1214 b [19], WASP- 44 b [12], WASP-23 b [13], WASP-15 b [20], WASP-19b • HATS582-003 was observed on 05.07.2012. A [14], Qatar-2 b [15], WASP-80 (in prep.). As an addi- clear eclipse was observed but the candidate was tional possibility offered by the GROND data, in six rejected as a triple due to V-shaped transit with cases we investigated the variations of the radius for very different depths in r0, i0, and z0. the planets in the wavelength ranges accessible to the instrument. We assembled planets’ transmission spec- • HATS582-005 was observed on 26.08.2012. The tra over the 370-2300nm wavelength range and com- transit was successfully recovered and the candi- pared these data to synthetic spectra, based on model date was recognized as a planet and renamed as atmosphere in chemical equilibrium, with P-T profiles HATS-3 [9]. assumed both planet-wide and day-side, and with dif- • HATS549-003 was observed on 11.10.2012, but ferent opacity characteristics (see an example in Fig. the transit ingress was observed nearly 1.33h 4). 4 9. Objects to be observed

(Objects to be observed with high priority should be marked in last column)

magnitude in Designation α (2000) δ (2000) spectral range priority to be observed

WASP-61 05h 01m 11.91s. −26◦ 030 14.900 V=12.5 medium WASP-62 05h 48m 33.59s. −63◦ 590 18.300 V=10.2 medium WASP-63 06h 17m 20.74s. −38◦ 190 23.800 V=11.2 medium WASP-64 06h 44m 27.61s. −32◦ 510 30.300 V=12.3 high WASP-66 10h 32m 54.00s. −34◦ 590 23.300 V=11.6 high WASP-67 19h 42m 58.51s. −19◦ 560 58.400 V=12.5 medium WASP-72 02h 44m 09.60s. −30◦ 100 09.100 V=10.9 high WASP-77 02h 28m 37.22s. −07◦ 030 38.400 V=10.3 high WASP-78 04h 15m 01.51s. −22◦ 060 59.100 V=12.0 high WASP-79 04h 25m 29.02s. −30◦ 360 01.500 V=10.0 high WASP-82 04h 50m 38.56s. +01◦ 530 38.600 V=10.1 high WASP-99 02h 39m 35.44s. −50◦ 000 28.800 V=10.1 high WASP-101 06h 33m 24.26s. −23◦ 290 10.200 V=10.1 medium HATS503-003 05h 22m 00.00s. −18◦ 250 00.000 V=13.9 medium HATS549-007 04h 40m 00.00s. −19◦ 100 00.000 V=14.8 medium HATS552-017 05h 52m 00.00s. −19◦ 010 00.000 V=15.1 medium HATS552-022 06h 03m 00.00s. −19◦ 020 00.000 V=10.1 high HATS554-009 06h 58m 00.00s. −19◦ 410 00.000 V=13.0 medium HATS582-006 20h 52m 00.00s. −25◦ 410 00.000 V=14.0 medium HATS579-017 19h 23m 00.00s. −20◦ 090 00.000 V=13.2 medium HATS579-023 19h 16m 00.00s. −19◦ 210 00.000 V=12.9 medium HATS579-026 19h 37m 00.00s. −22◦ 120 00.000 V=12.9 medium HATS581-081 20h 22m 00.00s. −24◦ 500 00.000 V=13.2 medium

5 10. Justification of the amount of observing time requested:

The ultimate goal of the present proposal is to use the GROND instrument to simultaneously obtain multi-band, high signal-to-noise differential photometry of complete planetary transit events, which will be analysed to measure the physical properties of the corresponding planetary systems. We want to observe ∼ 6 HAT-South planet candidates and ∼ 6 known TEPs (a possible list of targets is reported in 9.0; please, note that that the HATS targets are very hot planet candidates that have been found by the HATSouth consortium, of which the applicants are members, but are not yet published. Following the policy of the HATSouth collaboration, we have truncated their RA and Dec). At present roughly half of the ∼ 300 known TEPs do not have high-quality follow-up light curves, and so their properties are relatively uncertain. We are therefore conducting a long-term project to observe these objects. We also have access to the data of the Danish 1.52m telescope, which will be complementary to the GROND data. We require observations of at least two transits to obtain definitive results for a single planet (depending on the characteristics of individual targets). This is why our project has to run in survey style: we require a substantial investment of telescope time, which returns publishable results for a large number of objects. The number of the hours that we request is estimated considering the mean duration of a generic planetary transit and the necessity to observe each target at least 60 min before ingress and 60 min after egress, in order to obtain a stable out-of-transit baseline magnitude which is crucial for the accurate transit fitting model. 11. Constraints for scheduling observations for this application:

The scheduling constraints are very speciﬁc, since it is necessary to choose only nights where our targets undergo transit event. So, the ﬁnal choice of the targets will be done when we will know the P93 MPIA GTO periods. 12. Observational experience of observer(s) named under 2.3: (at least one observer must have sufficient experience) Luigi Mancini is an expert on precise transit photometry with medium-class telescopes. He has already observed planetary transits many times with the 2.5m INT, the CAHA 2.2m, the MPG/ESO 2.2m, the 1.54m Danish Telescope, the OAB 1.52m Cassini Telescope, and the CAHA 1.23m Telescope. He also used the FEROS spectrograph for RV measurements with the MPG/ESO 2.2m Telescope. Simona Ciceri has a very good observing experience of planetary transits with the CAHA 1.23-m, Cassini 1.52-m, Danish 1.54-m and the MPG/ESO 2.2-m Telescopes. 13. Observing runs at the ESO 2.2m-telscope (preferably during the last 3 years) and publications resulting from these Telescope instrument date hours success rate publications 2.2m GROND Oct 2011 ∼ 18 100% [12, 19] 2.2m GROND Jan 2012 ∼ 12 100% [7, 13] 2.2m GROND Feb 2012 ∼ 6 100% [8] 2.2m GROND Apr 2012 ∼ 34 100% [13, 14, 20, 15] 2.2m GROND Jun 2012 ∼ 6 100% [8] 2.2m GROND Aug 2012 ∼ 6 100% [9] 2.2m GROND Dic 2012 ∼ 6 100% [21] 2.2m GROND Jun 2013 ∼ 6 100% in prep.

6 14. References for items 8 and 13: [1] Southworth (2009): Homogeneous studies of transiting extrasolar planets - II. Physical properties, Mon. Not. Roy. Astron. Soc. 394, 272 [2] Christian, Pollacco, Skillen, et al. (2006): The SuperWASP wide-field exoplanetary transit survey, Mon. Not. Roy. Astron. Soc. 372, 1117 [3] Bakos, Hartman, Torres, et al. (2011): Planets from the HATNet project, “Detection and Dynamics of Transiting Exoplanets”, St. Michel l’Observatoire, France, Edited by F. Bouchy; R. Daz; C. Moutou; EPJ Web of Conferences, Volume 11, id.01002 [4] Alonso, Brown, Torres, et al. (2004): TrES-1: The Transiting Planet of a Bright K0 Star, The Atrophysical Journal 613, L153 [5] Borucki, Koch, Basri, et al. (2011): Characteristics of Planetary Candidates Observed by Kepler, The Atrophysical Journal 736, 19 [6] Bakos, Csubry, Penev, et al. (2013): HATSouth: a global network of fully automated and identical wide- field telescopes, Publications of the Astronomical Society of the Pacific 125, 154 [7] Penev, Bakos, Bayliss, et al. (2013): HATS-1b: a hot jupiter discovered by the HATSouth transit survey, The Astronomical Journal 145, 5 [8] Mohler, Mancini, Hartman et al. (2013): HATS-2b: a transiting extrasolar planet orbiting a K-type star showing starspot activity, Astronomy & Astrophysics 558, A55 [9] Bayliss, Zhou, Penev, et al. (2013): HATS-3b: an inflated hot jupiter transiting an F-type star, The Astronomical Journal 146, 13 [10] Southworth, Mancini, Maxted, et al. (2012): High-precision photometry by telescope defocussing. IV. Physical properties and transmission photometry of HAT-P-5, Mon. Not. Roy. Astron. Soc. 422, 3099 [11] Mancini, Southworth, Ciceri, et al. (2013): A lower radius and mass for the transiting extrasolar planet HAT-P-8 b, Astronomy & Astrophysics 551, A11 [12] Mancini, Nikolov, Southworth, et al. (2013): Physical properties of the WASP-44 planetary system from simultaneous multi-color photometry, Mon. Not. Roy. Astron. Soc. 430, 2932 [13] Nikolov, Chen, Fortney, Mancini, et al. (2013): Refined physical properties and g0, r0, i0, z0, J, H, K transmission spectrum of WASP-23b from the ground, Astronomy & Astrophysics 553, A26 [14] Mancini, Ciceri, Chen, et al. (2013): Physical properties, transmission and emission spectra of the WASP- 19 planetary system from multi-colour photometry, Mon. Not. Roy. Astron. Soc. 436, 2 [15] Mancini, Southworth, Ciceri, et al. (2013): Physical properties, starspot activity and transmission spectrum of the Qatar-2 planetary system from multi-colour photometry, submitted to A&A [16] Fukui, Narita, Kurosaki, et al., 2013: Optical-to-near-infrared Simultaneous Observations for the Hot Uranus GJ3470b: A Hint of a Cloud-free Atmosphere, The Atrophysical Journal 770, 95 [17] Copperwheat, Wheatley, Southworth, et al., 2013: Transmission photometry of WASP-12b: simultaneous measurement of the planetary radius in three bands, Mon. Not. Roy. Astron. Soc. 434, 661 [18] Fortney, Lodders, Marley & Freedman (2008): A Unified Theory for the Atmospheres of the Hot and Very Hot Jupiters: Two Classes of Irradiated Atmospheres, The Atrophysical Journal 678, 1419 [19] Harpsoe, Hardis, Hinse, et al. (2013): The Transiting System GJ1214: high-precision defocused transit observations and a search for evidence of transit timing variation, Astronomy & Astrophysics 549, A10 [20] Southworth, Mancini, Browne, et al. (2013): High-precision photometry by telescope defocussing. V. WASP-15 and WASP-16, Mon. Not. Roy. Astron. Soc. 434, 1300 [21] Zhou, Bayliss, Hartman, et al. (2013): The mass-radius relationship for very low mass stars: four new discoveries from the HATSouth survey, to appear in Mon. Not. Roy. Astron. Soc., arXiv:1310.7591

7 Tolerance limits for planned observations: maximum seeing: 300 minimum transparency: 50% maximum airmass: 2.0 photometric conditions: no moon: max. phase / 6 : 1/30◦ min. / max. lag: 0/0 nights