Microlensing search for extrasolar planets: observational strategy, discoveries and implications

The search for extrasolar Earth-like planets

The search for extrasolar planets has already detected rocky planets and several planetary candidates with minimum masses that are consistent with rocky planets in the habitable zone of their host stars. A low-resolution spectrum in the form of a color-color diagram of an exoplanet is likely to be one of the first post-detection quantities to be measured for the case of direct detection. In this paper, we explore potentially detectable surface features on rocky exoplanets and their connection to, and importance as, a habitat for extremophiles, as known on Earth. Extremophiles provide us with the minimum known envelope of environmental limits for life on our planet. The color of a planet reveals information on its properties, especially for surface features of rocky planets with clear atmospheres. We use filter photometry in the visible as a first step in the characterization of rocky exoplanets to prioritize targets for follow-up spectroscopy. Many surface environments on Earth have characteristic albedos and occupy a different color space in the visible waveband (0.4-0.9 μm) that can be distinguished remotely. These detectable surface features can be linked to the extreme niches that support extremophiles on Earth and provide a link between geomicrobiology and observational astronomy. This paper explores how filter photometry can serve as a first step in characterizing Earth-like exoplanets for an aerobic as well as an anaerobic atmosphere, thereby prioritizing targets to search for atmospheric biosignatures.

Several areas of stellar observations depend critically on nearly continuous observations of individual objects over very extended periods. Important examples are investigations of stellar oscillations to carry out asteroseismology, and the search for extra-solar planets. To meet this requirement we are establishing the SONG network, consisting of 8 sites with a 1-meter-class telescope with a suitable geographical distribution. These will be optimized for asteroseismology based on Doppler-velocity observations and the characterization of extra-solar planets with photometry, using gravitational microlensing. Funding has been obtained towards the construction of the prototype SONG telescope which will be set up on Tenerife, with first light expected in 2011. The full network will be established in parallel with the tests of the prototype and is planned to be operational in 2014.

Meeting announcements

ABSTRACTGIARPS (GIAno & haRPS) is an observing mode that allows having on the same focal station of the Telescopio Nazionale Galileo (TNG) both the high-resolution spectrographs, HARPS–N (visible, VIS) and GIANO–B (near-Infrared, NIR), working simultaneously. To date, GIARPS is the first and unique worldwide instrument providing cross-dispersed echelle spectroscopy at R= 50,000 in the NIR and 115,000 in the VIS over a wide spectral range (0.383−2.45 μm) in a single exposure. GIARPS is online since 2017 and it is used in a wide range of science cases, especially for the search of exoplanets around young and active stars and the characterization of their atmosphere. In the next future, it will be equipped with NIR absorbing cells to obtain high precision radial velocity (RV). Furthermore, a solar telescope (LOCNES, D=10 cm) will allow the use of GIANO-B to study NIR spectra of the Sun-like-a-star to have more hints on the influence of activity on RV and transmission spectroscopy.1. GIARPSGIARPS (Claudi et al 2017) is a TNG observing allowing the simultaneous use of the HARPS-N and GIANO-B spectrographs, exploiting a wide wavelength range (0.383 - 2.45 µm) with high-resolution (115,000 in the visible, 50,000 in the NIR) in a single exposure. GIARPS is the result of the refurbishment of GIANO from a fiber-fed spectrograph to GIANO-B directly fed by the same Nasmyth-B focus feeding HARPS-N, by means of a preslit.The light coming from the Nasmyth-B focus meets a dichroic that reflects the visible toward HARPS-N and transmits the NIR to GIANO-B. The dichroic is mounted on a motorized slide to select the preferred observing mode.GIANO-B dewar is rigidly connected to the fork of the TNG and does not add vibration modes to those generated by the telescope (jitter, tracking etc.). For the time being, GIARPS uses both the instruments for high precision radial velocity measurements exploiting the simultaneous reference technique with HARPS-N (Th–lamps) and GIANO-B (telluric lines) reaching in the NIR about 10 m\s for bright stars (H≤5 mag) and 70 m\s (H~9 mag). In future, it will be equipped with absorption cells (acethylene, ammonia and methane) to reach the better precision of 3 m/s.2. SCIENTIFIC RESULTS2.1 EXOPLANETARY SCIENCEIn the last few years, several works reported the contribution of GIARPS in the field of the search and characterization of extrasolar planets.The simultaneous RV collection in the VIS and NIR band allows discriminating between planetary and stellar signals, being the latter wavelength-dependent.Carleo et al. (2018) made use of several NIR RVs to rule-out the hot Jupiter around the 150 Myr old star BD+201790. With a similar method, in the framework of the GAPS2 program, Carleo et al. (2020) confirmed the presence of a hot Jupiter around the Hyades member HD285507 and demonstrated that the previously detected RV signal around AD Leo has stellar origin.GIARPS also provides suitable data for the atmospheric characterization of exoplanets. Guilluy et al. (2020) performed high-resolution transmission spectroscopy of the transiting hot Jupiter HD189733b aiming to detect the absorption signal of the helium triplet at 1083.3 nm, an useful diagnostic for extended and escaping atmospheres. They confirmed the result by comparing the helium feature with the one of the Halpha in the VIS to evaluate the stellar activity impact on the planetary absorption.Finally, Baratella et al. (2020) analysed a sample of intermediate-age stars (

The Exoplanet Tracker is a prototype of a new type of fibre-fed instrument for performing high precision relative Doppler measurements to detect extra-solar planets. A combination of Michelson interferometer and medium resolution spectrograph, this low-cost instrument facilitates radial velocity measurements with high throughput over a small bandwidth (~ 300 Angstroms), and has the potential to be designed for multi-object operation with moderate bandwidths (~1000 Angstroms). We present the first planet detection with this new type of instrument, a successful confirmation of the well established planetary companion to 51 Peg, showing an rms precision of 11.5m/s over five days. We also show comparison measurements of the radial velocity stable star, Eta Cas, showing an rms precision of 7.9m/s over seven days. These new results are starting to approach the precision levels obtained with traditional radial velocity techniques based on cross-dispersed echelles. We anticipate that this new technique could have an important impact in the search for extra-solar planets.

We present new radial velocity measurements of eight stars secured with the spectrograph SOPHIE at the 193-cm telescope of the Haute-Provence Observatory allowing the detection and characterization of new giant extrasolar planets. The host stars are dwarfs of spectral types between F5 and K0 and magnitudes between 6.7 and 9.6; the planets have minimum masses M_p sin i between 0.4 to 3.8 M_Jup and orbital periods of several days to several months. The data allow only single planets to be discovered around the first six stars (HD143105, HIP109600, HD35759, HIP109384, HD220842, and HD12484), but one of them shows the signature of an additional substellar companion in the system. The seventh star, HIP65407, allows the discovery of two giant planets, just outside the 12:5 resonance in weak mutual interaction. The last star, HD141399, was already known to host a four-planetary system; our additional data and analyses allow new constraints to be put on it. We present Keplerian orbits of all systems, together with dynamical analyses of the two multi-planetary systems. HD143105 is one of the brightest stars known to host a hot Jupiter, which could allow numerous follow-up studies to be conducted despite this is not a transiting system. The giant planets HIP109600b, HIP109384b, and HD141399c are located in the habitable zone of their host star.

Context. One of the most metal-rich open cluster of the Galaxy, NGC 6253 is a target of special interest in the search for extrasolar planets, the study of stellar populations, and the chemical/dynamical evolution of the Galactic disk. Aims. We present the results of two photometric campaigns and a VLT multi-epoch radial velocity survey toward the open cluster NGC 6253. We complement our analysis with photometric, proper motion, and radial velocity data available from previous studies of this cluster, and analyze three planetary candidates found in the field of NGC 6253. Methods. We derived homogeneous radial velocity measurements for stars located at the turn-off, sub-giant, red-giant branch, redclump, and blue straggler regions of the cluster. We also analyzed a comparison sample of surrounding field stars. Spectra were obtained with the UVES and GIRAFFE spectrographs at the VLT during three epochs in August 2008. Results. The three UVES measurements acquired for our brightest transiting candidate (V = 15.26) are all consistent within their errors (200 m/s), but were acquired at very similar orbital phases. The mean radial velocity of this object is not consistent with the cluster recession velocity, which rules out cluster membership except in the case of a binary system. This star is worth further analysis with high-precision spectroscopy. For our faintest candidate (V = 18.247), we were able to exclude the observed transits being caused by a close-by stellar companion, but more precise measurements will be needed to derive an orbital fit and to study other possible scenarios. For the remaining candidate, no measurements were acquired probably because of bad fiber positioning. The mean radial velocity of the cluster is (RV cl cl ) = (-29.11 0.85) km s -1 . Using both radial velocities and proper motions, we identified 35 cluster members. Our results are in good agreement with past radial velocity and photometric measurements. Furthermore, using our photometry, astrometry, and spectroscopy we identified a new eclipsing binary system member of the cluster. Conclusions. We discussed the possibility of detecting substellar companions (brown dwarfs and planets) with the radial velocity technique (both with UVES/GIRAFFE and HARPS) around turn-off stars of old open cluster. We isolated 5 stars that are optimal targets for searching for planetary mass companions with HARPS. Our optimized strategy minimizes the observing time requested to isolate and followup on the best planetary candidates in cluster with high-precision spectrographs, an important aspect given the faint target stars.

The astronomical technique of gravitational microlensing provides new opportunities to make measurements which are difficult or impossible by other methods, or which are complementary to those obtained more directly. These include detection of dark matter, determination of galactic structure, measurement of limb darkening of stars, and searches for extra-solar planets. The technique is best suited to the southern sky, and several observations have been made from Australasia. A sample of these observations is described here. A case is also made for a telescope at the Antarctic dedicated to gravitational microlensing.

Developments in the search for extra-solar planets via gravitational microlensing by the Japan/New Zealand group MOA are discussed. The use of the Kaláka cluster computer is introduced and preliminary results presented.

Search for Extra-Solar Planets and Dark Matter by Gravitational Microlensing

What does it take to consider a planet potentially habitable? If a planet is suitable for life, could life be present? Is life on other planets inevitable? Searching for Habitable Worlds answers these questions and provides both the general public and astronomy enthusiasts with a richly illustrated discussion of the most current knowledge regarding the search for extrasolar planets. Nearly everyone wants to know if we are alone in the universe. This book might not have the answers, but shows where we should look. This book is a fun and accessible book for everyone from middle schoolers to amateur astronomers of all ages. The use of non-technical language and abundant illustrations make this a quick read to inform everyone about the latest movement in the search for other planets that we might be able to inhabit. After a brief discussion on why humans are hard-wired to be curious, and to explore the unknown, the book describes what extrasolar planets are, how to detect them, and how to pin down potential targets. In addition, a data-driven list of the best candidates for habitability is profiled and the next generation of exoplanet-hunting scientific instruments and probes are identified.

(Abridged) Searching for planets around stars with different masses probes the outcome of planetary formation for different initial conditions. This drives observations of a sample of 102 southern nearby M dwarfs, using a fraction of our guaranteed time on the ESO/HARPS spectrograph (Feb. 11th, 2003 to Apr. 1st 2009). This paper makes available the sample's time series, presents their precision and variability. We apply systematic searches and diagnostics to discriminate whether the observed Doppler shifts are caused by stellar surface inhomogeneities or by the radial pull of orbiting planets. We recover the planetary signals corresponding to 9 planets already announced by our group (Gl176b, Gl581b, c, d & e, Gl674b, Gl433b, Gl 667Cb and c). We present radial velocities that confirm GJ 849 hosts a Jupiter-mass planet, plus a long-term radial-velocity variation. We also present RVs that precise the planetary mass and period of Gl 832b. We detect long-term RV changes for Gl 367, Gl 680 and Gl 880 betraying yet unknown long-period companions. We identify candidate signals in the radial-velocity time series and demonstrate they are most probably caused by stellar surface inhomogeneities. Finally, we derive a first estimate of the occurrence of M-dwarf planets as a function of their minimum mass and orbital period. In particular, we find that giant planets (m sin i = 100-1,000 Mearth) have a low frequency (e.g. f<1% for P=1-10 d and f=0.02^{+0.03}_{-0.01} for P=10-100 d), whereas super-Earths (m sin i = 1-10 Mearth) are likely very abundant (f=0.36^{+0.25}_{-0.10} for P=1-10 d and f=0.35^{+0.45}_{-0.11} for P=10-100 d). We also obtained eta_earth=0.41^{+0.54}_{-0.13}, the frequency of habitable planets orbiting M dwarfs (1<m sin i<10 Mearth). For the first time, eta_earth is a direct measure and not a number extrapolated from the statistic of more massive and/or shorter-period planets.

We evaluate the direct detection of extrasolar giant planets with a two-aperture nulling infrared interferometer, working at angles θ < λ/2B and using a new ratio-of-two-wavelengths technique. Simple arguments suggest that interferometric detection and characterization should be quite possible for planets much closer than the conventional inner working angle, or angular resolution limit. We show that the peak signal from a nulling infrared interferometer of baseline 40 m will often occur inside the null and that the signal variations from path difference fluctuations will cancel to first order in the ratio of two wavelengths. Using a new interferometer simulation code, we evaluate the detectability of all the known extrasolar planets as observed using this two-color method with the proposed Fourier-Kelvin Stellar Interferometer (FKSI). In its minimum configuration FKSI uses two 0.5 m apertures on a 12.5 m baseline and a ±20° field of regard. We predict that ~7 known extrasolar planets are directly detectable using FKSI, with low-resolution spectroscopy (R ~ 20) being possible in the most favorable cases. Spaceborne direct detection of extrasolar giant planets is possible with ~12 m baselines and does not require the much longer baselines provided by formation flying.

Various techniques are being used to search for extra‐solar planetary signatures, including accurate measurement of positional (astrometric) displacements, gravitational microlensing, and photometric transits. Planned space experiments promise a huge increase in the detections and statistical knowledge arising from transit and astrometric measurements. In contrast, imaging of even nearby Earth‐mass planets in the habitable zone and the measurement of their spectral characteristics, typified by the TPF and Darwin missions, represents an enormous challenge. A number of proposed precursors aimed at exploiting coronagraphy or occultations are being studied. Beyond TPF/Darwin, Life Finder would aim to produce confirmatory evidence of the presence of life, while an Earth ‘imager’, some massive interferometric array providing resolved images of a distant Earth, appears only as a distant vision. A 10 nas astrometric mission would detect ‘Earths’ systematically out to 100 pc.