All posts by Pale Red Dot

Terrestrial Planets over the Next Decade

By Don Pollaco, Warwick University, UK

There can be no doubt that NASA’s Kepler mission has been a resounding success. In particular, much of what we know about rocky planets has come from this mission. After saying that, ground-based radial velocity surveys had already indicated the existence of super-Earths—a class of planet not found in our solar system (ignoring Planet 9!), and the first exo-rocky planet discovered was found through the French-ESA CoRoT mission (Corot-7b). The list of “firsts” from Kepler is truly amazing:

  1. Planetary size distribution
  2. The commonality of multi-planet systems
  3. The application of transit timing techniques to derive planetary masses and the recovery of unseen components
  4. The detection and modelling of the first circumbinary systems
  5. The diversity of low mass planets
  6. The evaporation and breakup of small planets

and so, while some results are less good, e.g. estimate of eta-Earth (number of habitable zone planets per star) and the masses of low-mass planets, Kepler’s place in history is assured. To me though, Kepler’s greatest result is really the ubiquity of exoplanets; specifically small planets.

Almost as impressive has been Kepler’s contribution to the proving of stellar asteroseismology. Whilst these techniques had been applied to the Sun and individual stars, Kepler has been used to derive stellar parameters for hundreds of stars at a level never before achieved en masse.

Kepler Small Planets

Kepler has given us a tantalizing first glimpse of the small/rocky planet population and some of the results have been absolutely awesome (Figure 1). For example, masses for the fantastic seven planet Kepler-11 system have been derived through modelling the gravitational perturbations giving rise to the transit time variations, and show these planets are much bigger than expected for their masses—maybe they are mini gas planets or have fluffy extended atmospheres.

Figure 1. The known small planet population in the mass-radius plane (x-axis’ units are Earth masses) compared to different compositions and compared to rocky planets in our solar system There is far more diversity than originally expected.

At the other extreme is Kepler-10c. Kepler-10b (mass 3.33ME, radius 1.47RE, Period 0.84d) was well known as Kepler’s first rocky planet, and spectroscopic observations from the ground with HARPS-N on La Palma not only confirmed this, but also detected the stellar reflex motion from the long period Kepler-10c component. Surprisingly, the mass turned out to be 17.2ME, but the Kepler (2.3RE) radius suggested we were still most likely looking at a massive super-Earth. Given that we struggle to understand the internal structure of the Earth, we are quite mystified to explain that of Kepler-10c. These results and others lead us to believe the small planet population is much more diverse than we originally believed.

When Kepler was being designed, it was generally agreed that there would be little variation of compositions in this population, so that from a measurement of planetary radius its mass could be directly inferred. Consequently, it was assumed that there would be little need for follow up observations. Kepler showed us the need to determine the planetary mass directly.

Radial Velocity Surveys: Masses of Kepler Planets

Since the first discovery of a planet around a Sun-like star (Mayor and Queloz 1995), radial velocity surveys—searching for the reflex motion induced in the star—were often the most efficient discovery technique. Compared to the transit method’s strict requirement on the orbital geometry, radial velocity detection is far more lenient. However, without knowledge of the orbital inclination to our line of sight, all we can determine is the planetary minimum mass. Basically, from radial velocity information alone we can learn about the planetary orbit, but essentially nothing about the planet itself.

Radial velocity information is most useful when it is used alongside transit data. With radius and, most importantly, orbital information coming from the light curve modelling, solutions of the equations of motion can give an accurate planetary mass. Thus, we can get an accurate estimation of the bulk density/composition of a planet. What should be emphasized here is that to derive the planetary mass and radii requires better accuracy in the stellar parameters; in fact, for the best transit light curves knowledge of the host star is often the factor limiting that of the planetary component. The study of exoplanets has led to a renaissance in stellar research and especially the proving of asteroseismology.

The low brightness of the Kepler field stars and the prevalence of small planets is a double whammy for our studies of the masses of small planets—the small reflex motion and lack of stellar photons make mass measurements at best somewhat challenging. So while the Kepler photometry has produced highly accurate relative radii, even the brightest Kepler host stars are challenging targets for radial velocity work. It is ironic that the planets with the most accurate accepted masses are massive planets found from ground-based transit surveys such as SuperWASP or HAT.

As a consequence, researchers have developed our ability to model gravitation perturbations detectable through transit timing variations (as noted earlier) and this is how most Kepler planetary masses have been determined. This has the advantage that they can be derived from the light curve alone and with apparently small errors, but is possible for only a small fraction of the planets. There is still some controversy surrounding the use of masses derived in this way and maybe more importantly in the quoted errors. Maybe this will improve in the future.

However, one of the big lessons from Kepler (and the ongoing K2 surveys of course) is that we need a host star population as bright as possible so we can derive masses, make planetary atmosphere observations, etc. So given this, what does the future hold?

Looking forward—the Transit Roadmap

For exploring the inner parts of solar systems, and in particular the habitable zones, for the next 10–15 years it is likely that transits of bright stars that allow radial velocity observations to be made will dominate (Figure 2). That’s not to say that other techniques and regions of the parameter space will not be important—they will. For example, with SPHERE and GPi we are taking our first steps with dedicated and optimized instruments capable of direct planet detection—at least of luminous, young and massive planets. JWST may also be capable of this. Gaia and various microlensing space missions such as WFIRST (~2025) or EUCLID (2021) will allow us to statistically explore the outer parts of solar systems.

Figure 2. The funded transit roadmap showing facilities that are used for detection and bulk characterisation. Some of the facilities here can also be used for atmospheric characterisation.

In terms of transit experiments, we have a crop of ground-based experiments—including the new NGTS, and the re-tasked Kepler K2 surveys. While still at an early stage, NGTS is proving capable of routinely detecting dips which could be due to Neptune-sized objects. Various experiments have been deployed targeting M dwarf stars, where the low intrinsic brightness and small star size mean that ground based photometry would even be capable of detecting Earth-sized planets in orbits of a few days; corresponding to the habitable zones of the feeblest stars.

In general, finding small planets (smaller than Neptune, say) in habitable zones is a difficult task and is best done from space. This not only avoids limitations in photometric accuracy from the Earth’s atmosphere, but also the interruptions caused by the day/night cycles. Even still, as we push to higher and higher accuracies stellar activity becomes a bigger issue with less stars being suitable for radial velocity work. However, understanding stellar activity is an area of much research and there is hope that small radial velocity signals will be detectable against the activity signal in the future. Nonetheless, we are fortunate that both NASA and ESA have recognized the need for new surveys and we have a series of missions that have transit detection at their heart.

CHEOPS is due for launch in 2017 and is ESA first “Small” satellite. This Swiss led mission is designed to look at objects one at a time. CHEOPS has two science drivers:

  1. The follow up of known planets discovered from radial velocity surveys and especially those targets thought likely to transit, and
  2. High accuracy light curves of transits from other surveys, notably NGTS.

So, while CHEOPS is not a survey instrument it will produce extremely accurate photometry of known planets and hence bulk densities. CHEOPS also has many other potential uses such as monitoring transits for timing variations etc.

NASA’s Transiting exoplanet Survey Satellite, TESS, will be launched around the end of 2017. TESS will be orientated into a highly eccentric and inclined orbit which reaches almost to the lunar orbit. For most of the 27 day orbit the satellite will be far from the Earth, enabling accurate photometry. The clever orbit and observation strategy results in sections of the sky being monitored for 27 days before moving to the next section. These sections overlap at the Ecliptic poles and so a small region is monitored for as long as ~1 year. Given this, it is likely that TESS will find many single transiting systems which would benefit from CHEOPS observations.

TESS is aimed at surveying the nearest and brightest stars (mag) and is therefore preferentially examining M dwarfs. These low luminosity stars have habitable zones close in (periods as short as a week or so for the coolest objects). Furthermore, as these stars are quite small the detection of small planets can be achieved easier. Being extremely red objects they are likely to be ideal targets for the JWST and it is likely that the first observations of the atmosphere of a habitable zone planet will come from TESS.

The Future: ESA’s M3 PLATO Mission

Over the years, there has been a succession of transit survey concepts studied by ESA, but in 2014, PLATO was finally selected as the “Medium 3” mission with launch date in 2024. PLATO was designed from the outset to characterize habitable zone rocky planets with Sun-like host stars that are bright enough for observation with the new generation of radial velocity spectrograph’s such as ESPRESSO at ESO’s Very Large Telescope (VLT) in Chile. PLATO is a multi-telescope system which provides a huge field of view (>2,200 square degrees—about 20 times that of Kepler) with excellent sensitivity and it will be stationed in a thermally stable environment at the L2 point, several million kilometers from Earth. While the dynamic range is from 4–13 magnitude, most of the interesting science will be for stars with magnitudes allowing asteroseismic characterization of accurate stellar parameters including their age. Figure 3 shows the predicted rocky planet catch for stars that can be fully characterized through asteroseismology compared to those from Kepler and TESS.

Figure 3. Simulations of PLATO transit signal detection performance (in green) for super-Earth planets (less than 2RE) for stars brighter than 11 mag, hence with RV follow-up and host star asteroseismology possible. For comparison, Kepler results are shown (in blue, Fressin et al. 2013) and expected yields for TESS (in red) assuming 27 day observing coverage per field and 2% of the sky observed for 1 year

The time requirement for the ground-based follow up will be almost entirely driven by the smallest, longest period, planets and will represent a significant investment by the astronomical community. For some of the multi-planet systems, masses will also be available from models of any transit timing variations. While PLATO will certainly produce lots of interesting and no doubt unique systems and maybe even moons, rings, etc., the real PLATO reward will be the database of uniformly characterized planetary systems that can be used for future theoretical and observational experiments.

By the end of the next decade, we will have fully characterized hundreds of systems containing rocky planets. Many of these will be bright enough to have their atmospheres examined with the instruments of the day. The database of PLATO systems with known ages will allow us to take the first steps in comparing the observed planet population with theoretical studies, hence throwing light on the important processes that are sculpting the architectures of these systems. In many ways PLATO can be considered the descendant of Kepler and indeed one of the options for PLATO is to revisit the Kepler field to examine the variations in transit timing variations accumulated after a delay of some 15 years.

We live at a very fortunate time. Kepler has opened the window and shown us some of the landscape. The new missions will enable us to make great gains in comparative planetology so that we can understand our place in the Universe.

Dr Don Pollacco, astro-physicist and planet hunter from Queens University, Belfast.

About the author. Don Pollaco is a Professor of Astronomy at Warwick University, UK. He was awarded his PhD in 1990 from St Andrews University. From 1990–1995 he worked as a PDRA and then lecturer at St Andrews and Liverpool John Moores Universities. Between 1995-2000 he was based at the Isaac Newton Group of Telescopes (ING) La Palma. His PhD and postdoctoral studies were concerned with evolved stars and binary systems. From 2000–2012 he worked at Queens University Belfast developing the exoplanet group there. During this period he led the development as PI of the SuperWASP Project and the initial development of NGTS. Since arriving at Warwick in 2012 he has been the Science Coordinator for ESA’s PLATO mission.



Big projects to unveil the birth, life, and death of a Pale Red Dot

By Jorge Lillo Box, European Southern Observatory (ESO)

Like a person, planets are born, evolve rapidly in the early stages of their lives, and spend most of their time interacting with others in their surroundings (in this case stars, other planets, comets, asteroids, etc.). At last, they die in a joint evolution with the system where they lived. The large crop of extrasolar planets discovered to date (around two thousand) is providing valuable information about how exactly these processes take place. But there are still many open questions that are key to understanding the whole picture. Starting from a planet’s birth and finishing with its death, I will briefly review some big projects and facilities aimed at answering these crucial questions.

Planets are byproducts of stellar formation. Stars are formed after the collapse of a molecular cloud. The result of this process is a massive object (the star) surrounded by a circumstellar disc composed of gas and dust. This disc is indeed the incubator where planets will be formed. However, the exact mechanism of planet formation is still a mystery, with different theories trying to explain the process and to conjugate theory and the observations. A property that seems to have a key role in planet formation is the amount of gas and its lifetime in the disc. Also, the amount of warm water, and in general the chemical contents available in the disc will determine the type of planets that can be formed. Two key projects using data from the Herschel mission of the European Space Agency (ESA) aim at characterizing these parameters in the different stages of planet formation: GASPS and DUNES. They are producing impressive results with the detection of warm water vapor in these protoplanetary discs, a crucial ingredient linked with planet formation and the development of life. Additionally, the observations carried out by the ALMA radio-interferometer (Chile) are shedding light on the formation process, detecting protoplanets in the first stages of their live as well as possible signatures of multi-planetary formation.

ALMA image of the protoplanetary disk around HL Tauri. The image shows clear dark rings that could be due to the presence of forming planets, although other theories (not involving planets) have also been proposed to explain them. Credits: ALMA (ESO/NAOJ/NRAO).

During the process of forming a planet within a protoplanetary disc, other minor objects are also created. Moons, comets, asteroids, and minor planets are also by-products of this process and could play a key role in the subsequent evolution of the planetary system, as well as being crucial for the development and support of life. For example, we know that tidal forces induced by the Moon on our Earth have an important role in transporting heat from the equator to the poles, contributing to the climate patterns of our planet. Similarly, in other extrasolar systems, these objects may exist and play similar or even more important roles. Additionally, the properties of their orbits (inclinations, eccentricities, etc.) are a direct consequence of the dynamical evolution of the system during its first stages. Hence, the detection of minor bodies in extrasolar systems will contribute to our knowledge on planet formation and evolution, and potentially the evolution of life. The HET and TROY projects aim at detecting these minor objects. First, the HET project has the challenging goal of detecting the first exomoons—natural satellites orbiting around known planets. They have obtained different candidates, although no confirmation has been published as for today. The TROY project aims at detecting exotrojan planets—bodies co-orbiting with known extrasolar planets in the stability points of their orbit. In the Solar System, we know that a cloud of trojans inhabits the Lagrangian points L4 and L5 of Jupiter’s orbit. Indeed, even our Earth has a long-term 300-meter diameter object co-orbiting with us.

Illustration of the minor bodies in the inner part of the Solar System, including Jupiter trojans and the main asteroid belt. These objects are byproducts of planet formation and have key information about that process. Detecting them in extrasolar systems may help us to understand the early evolution of planetary systems. Credits: NASA (Creative Commons).

On the other side, important space missions are discovering large amounts of exoplanets with which we can start doing statistics of planet populations. For instance, thanks to NASA’s Kepler mission, we now know that solar-like stars in our Galaxy harbor on average 0.77 earth-size planets. This is a crucial discovery since it tells us that earths are more or less commonly formed in the Universe. In the forthcoming years, new space missions such as TESS, CHEOPS, PLATO, Gaia, or JWST will each contribute to improve these numbers by detecting, and characterizing, extrasolar systems in other niches (for example, long-period planets).

The end of the story, as it happens in our own lives, is tragic. After several billion years, the host star exhausts its internal fuel (hydrogen) and starts to contract, while the external layers expand, making the star several times bigger than it was during its adult phase—becoming a red giant. The consequence of this process for the surrounding planets can be traumatic and catastrophic, possibly being engulfed by the star after a spiraling in-fall. But some of them can still survive. Determining the conditions for a planet to be engulfed by its host star is still a matter of debate. It is important to note that this process will also take place in our Solar System (although in several billion years). Hence, it is crucial to understand how planets die, and under which conditions, to know the future and the expiration date of our Earth. Several projects like EXPRESS, TAPAS or JOTA are currently looking for planets orbiting giant stars in order to contrast the theoretical predictions with actual data to shed light on the end of planetary systems.

An artist’s impression of HD 189733 b showing rapid evaporation of the atmosphere. Credits: NASA’s Goddard Space Flight Center (Creative Commons license).

A great technological and scientific effort is being put in to the study of all these processes. Understanding how planets are formed, evolve, and interact with other bodies in the system along their lives and finally finish their lives, is crucial to understanding our own world. The Pale Red Dot project is contributing to this by trying to detect the closest planetary system that we can find, a cousin of our own Solar System. Who knows what surprises this work will  bring? Just a few months left to get the answer…

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Dr. Jorge Lillo-Box

About the author.

Dr. Jorge Lillo-Box is a fellow at the European Southern Observatory (Santiago de Chile). Jorge studied Physics at the Complutense University and University of La Laguna. Afterwards he moved to the Astrobiology Center (INTA-CSIC, Madrid) where he got his PhD in 2015. Since last year he is settled in Chile where, if he is not pointing to a star at the Paranal Observatory, he would be delving into the study of the evolution of planetary systems in the last stages of their lives and in the detection of minor bodies through the TROY project. Among the several planets he has discovered in different niches, we highlight the first planet transiting a giant star or the closest planet to a host star ascending the Red Giant Branch, Kepler-91b.

Entre el ocaso y el alba con el gemelo norteño de HARPS

Por Zaira M. Berdiñas, Instituto de Astrofísica de Andalucía (IAA-CSIC)

Los observatorios son los laboratorios de los astrónomos, o mejor dicho, son nuestra ventana al Universo, que es El Laboratorio, con mayúsculas.

¿Conoces a alguien que, al mirar al cielo de noche, diga: “¡bah! no me gusta”? Yo no, pero también es cierto que a menudo la gran cantidad de luz de nuestras ciudades no nos da oportunidad de comprobar cual sería realmente la reacción; y quizá también por eso la inmensidad del Universo no es algo en lo que pensemos en nuestro día a día. Por eso, cuando conocemos a alguien con curiosidad por nuestra “estrellada profesión” nos suele preguntar –con una mezcla de curiosidad y extrañeza– “¿Cómo decidiste hacerte astrofísico?”. Cómo se desarrolla la vida en un observatorio puede causar la misma sensación de extrañeza y desconocimiento. De hecho, creo que ni mi madre sabe muy bien lo que hago allí arriba –¡no te enfades, mamá!– por eso en este artículo voy a describir un poco como es la rutina diaria en la montaña.

Comenzando el viaje en el aeropuerto de Granada. Créditos: Zaira M. Berdiñas.

Como muchos otros viajes, este comienza en el aeropuerto. Pero espera, eso no es del todo justo, porque antes de emprender el camino al observatorio ya se ha hecho gran parte del trabajo. Un par de veces al año, los telescopios ofrecen sus noches de observación en lo que denominan “llamamiento de propuestas”. En esos periodos los astrónomos deben estrujar sus cerebros y competir para escribir el mejor proyecto científico. El tiempo en los telescopios es caro y solo aquellos que demuestren que harán el mejor uso de ellos, tendrán la oportunidad de usarlos. Los “comités de asignación de tiempo”, que están formados también por astrónomos, deciden qué propuestas se aceptan y cuáles no. Así que estoy aquí, en el aeropuerto, lo que quiere decir que nuestro proyecto pasó el corte (¡yupi!). Tras un vuelo de 3 horas aterrizo en la isla de La Palma; quizá pienses que ya casi he llegado, pero aún me separan del Observatorio del Roque de los Muchachos unos cuantos cientos de curvasCarlos el conductor, y tras este zigzagueante viaje también mi amigo, me deja en la Residencia. Ésta es el núcleo de la vida en el observatorio: aquí es donde puedes ver astrónomos desayunando muy tarde,  cenando muy pronto, durmiendo durante el día o incluso jugando al ping-pong en su tiempo libre. Pero ya son las 4 de la tarde según mi reloj y no tengo tiempo que perder antes de que se ponga el Sol. Cojo un coche y conduzco hasta el Telescopio Nazionale Galileo (TNG), donde Vania, mi astrónoma de apoyo, me está esperando en la sala de control del telescopio para explicarme cómo configurar el instrumento que voy a usar para tomar mis datos: HARPS-N.

Izquierda: Telescopio Nazionale Galileo (TNG). Derecha: Sala de control localizada en la planta baja del edificio del telescopio. Las pantallas de la derecha las usa el operador del telescopio para controlar las condiciones atmosféricas y los parámetros del telescopio. Las pantallas de la izquierda son para manejar el instrumento, HARPS-N. Créditos: Zaira M. Berdiñas.

De la misma forma que Pale Red Dot usa HARPS, instalado en el Observatorio de La Silla (Chile), para tomar los datos de velocidad radial de Próxima Centauri, esta noche yo voy a usar HARPS-N, su gemelo en el hemisferio norte, para buscar planetas alrededor de otras estrellas rojas. Una vez que Vania termina sus explicaciones y después de inicializar y calibrar el instrumento, vuelvo rápidamente a la Residencia, ceno algo, guardo mi “super-snack” para la madrugada, leo algunos e-mails de mi equipo deseándome un cielo despejado, y conduzco hasta el telescopio con el Sol poniéndose a mi espalda. De camino, la cúpula abierta me dice que Daniele, el operador del telescopio, ya está listo para comenzar a observar. Apenas una hora después del crepúsculo, el cielo ya está lo suficientemente oscuro para comenzar con el procedimiento de enfoque del telescopio: la noche ha comenzado.

Telescopio Nazionale Galileo con su cúpula abierta en mi camino desde la Residencia. Créditos: Zaira M. Berdiñas

Me paso el resto de la noche observando mi lista de estrellas. Lo que hago es enviar comandos de observación para apuntar el telescopio y comenzar la exposición, mientras, compruebo que los espectros que voy tomando son de buena calidad. Durante toda la noche Daniele, que está a mi lado, controla las condiciones climáticas y los parámetros del telescopio desde unas nueve pantallas. Son casi las 2 de la mañana y le toca el turno a la estrella más débil de mi lista. Como ésta necesita una exposición más larga, me da la oportunidad de salir fuera y disfrutar de uno de los cielos más increíbles que puedes contemplar y, por qué no, de tomar unas cuantas fotos.

Fotografía de la Vía Láctea y el Telescopio Nazionale Galileo, hecha mientras se toma un espectro de larga exposición en el telescopio. Créditos: Zaira M. Berdiñas.

Tras casi 10 horas y más de un café, comienza a amanecer. Desconectamos todos los sistemas y conducimos hasta la Residencia, siempre con las luces apagadas para no molestar a colegas que puedan estar realizando aún alguna prueba de última hora. Y ya hemos acabado, los datos se analizarán durante los próximos meses, pero ahora son las 7 de la mañana, la noche ha terminado oficialmente, y lo único que me espera ahora mismo es mi cama. ¡Buenos días!

Zaira M. Berdiñas

Sobre la autora.

Zaira M. Berdiñas es doctoranda de último año y trabaja en el grupo del espectrógrafo CARMENES en el Instituto de Astrofísica de Andalucía. Su investigación se centra principalmente en la búsqueda de exoplanetas compactos y de pulsaciones en enanas de tipo espectral M usando espectrógrafos de velocidades radiales alimentados por fibras ópticas. En concreto, lidera las campañas observaciones con HARPS-N del proyecto Cool Tiny Beats, del que nació Pale Red Dot. Zaira también está activamente involucrada en el desarrollo de instrumentación. En este sentido, es parte del equipo de desarrollo del “Radial Velocity Corrector (RVC)”, una alternativa a los métodos de “scrambling” para espectrógrafos de velocidades radiales alimentados por fibras de alta precisión que no están térmicamente estabilizados.

Planetary transits: how can one measure the mass, size, density, and atmospheric composition of a planet one cannot even see?

Finding transiting planets

Our Solar System is shaped like a rather flat disk: all the major components are very close (to within a few degrees) to some imaginary “average” plane. Indeed, most (but not all) planetary systems are flat, so we can imagine other planetary systems as roughly disk-shaped. Relative to our own Solar system some of these flat systems will be seen “face on”, some will be “edge on”, and most will be somewhere in between.

One result of this randomness is that only a small minority of these systems will be oriented in such a way that their orbital plane is close to our line of sight (i.e. “edge-on”)—but this serendipity has multiple wonderful results indeed! Planets in such a system will seem to pass, or transit, in front of their host star once every orbit—as seen from earth—blocking a small fraction of the host star’s light for a short while in a “mini Solar eclipse”. This, as we will see below, allow us to both detect new exoplanets and learn a great deal about them.

Now, since stars appear like (very small) luminous disks, to a good approximation if half of the stellar disk is blocked by something opaque then we will see that star’s light diminish by half—this is what exoplanetary transits are all about. Firstly, we may ask: how small or large will this “mini eclipse” be? It is useful to have some examples: a Jupiter-like planet is about 10% the diameter of the Sun, so it can block about 1% of the Sun’s light (since the area of a circle is proportional to its diameter squared). Reversing this relation, if an astronomer finds a 1% deep transit-like dimming of a far-away star, he/she will conclude that the transiting object is approximately 10% the diameter of the host star—without ever measuring the size of the planet by an image that actually resolves the planet (obtaining such an image will require an unrealistically large telescope with a primary mirror about a kilometer in diameter).

Now, a 1% dimming of a star is something one can measure from the ground—so ~15 years ago multiple surveys started looking for such large planets (scale of Jupiter in size)—monitoring millions of stars every few minutes for months, and even years, on end. Why millions? Because not all stars are bright enough or stable enough to allow the detection of a 1% transit, and only a fraction of them actually host a large planet close-in to its host star (a so-called “Hot Jupiter”), and only a fraction of those are aligned close to our line of sight… so one has to start with millions of stars to find a handful of transiting planets. Processing this large amount of data requires sophisticated algorithms and a large degree of automation, and so quite some time passed before astronomers found out how to do this the right way. Today, a few hundreds of these ground-based detected transiting planets are known.

Top: As planets revolve around their star they exhibit phases akin to the phases of the Moon, since we see variable parts of their day or night sides throughout their orbit. This picture, however, is not what one can see with a telescope. Bottom: the observed flux (=brightness) of a star hosting a transiting planet. We will see different amount of flux depending on the part of the planetary orbit: when the planet goes behind the star we will see just the star alone. At all other phases we will see a both the star and the planet , and the the latter will also block some of the star's light during transit.
Top: As planets revolve around their star they exhibit phases akin to the phases of the Moon, since we see variable parts of their day or night sides throughout their orbit. This picture, however, is not what one can see with a telescope. Bottom: the observed flux (=brightness) of a star hosting a transiting planet. We will see a different amount of flux depending on the part of the planetary orbit: when the planet goes behind the star we will see just the star alone. At all other phases we will see both the star and the planet, and the latter will also block some of the star’s light during transit.

The space revolution

Unfortunately, detecting transiting planets much smaller than Jupiter is very difficult from the ground, if not impossible: an Earth-sized planet is a about tenth the diameter of Jupiter, or 1/100 the diameter of the Sun, so if can only impart a transit which is about 0.01% deep, much too small to be detected from ground-based observatories, which have to combat things like day/night cycles, weather, atmosphere, variable temperatures, etc.—all of which make precise measurements difficult. Fortunately, space-based observatories simply avoid all of these disturbances, so even by simply placing the exact same equipment in space one immediately gets much more precise measurements due to the very stable environment available in space—with no day/night cycles, no weather, no atmosphere etc. Indeed, NASA’s Kepler mission did more than that: the instrument aboard the Kepler spacecraft was highly optimized to the precise measurement of stellar brightness that does allow the detection of small Earth-like planets despite their small transit depth and long period. This, in turn completely revolutionized the exoplanets field.

Before Kepler about 300 exoplanets were known from all transit and radial velocity surveys combined, while Kepler alone found (as of today) over 1,000 confirmed planets, with >3,000 more candidates still waiting confirmation. Importantly, the kinds of planets Kepler found were very different from the giant planets usually found by other transit and radial velocity surveys; it found that most planets are small, with the most common type of planet only 2-3 times the diameter of the Earth. In fact, so many planets were found that it is now understood that most stars have at least one planet, and likely multiple planets, around them.

More than just detecting planets

Indeed, finding lots of planets is a lot of fun, but there is more—much more—to transiting planets than that. For starters, by combining the mass (from instruments like HARPS that measure precise radial velocity) and radius (from transits), one can easily calculate the planet’s mean density, which in turn can tell us something about the bulk composition of the planet. It was found that planets are indeed far more diverse than anyone had ever suspected before—with planets having densities spanning about two orders of magnitude; some planets are almost all high-density iron while others are less dense than Styrofoam, virtually devoid of solid material and probably all made of light elements like hydrogen and helium.

One of the early successes of the transit method stemmed from the understanding that the top layers of the planetary atmosphere are rarefied enough so they are not completely opaque. This means that as the planet transits the host star, some of the stellar light that passes through these layers is not completely absorbed and actually makes it through to us, and now it carries some information about the conditions that exist in these upper layers of the planetary atmosphere in its spectrum. By subtracting the on- and off- transit spectra one can isolate this faint planetary contribution to the overall light coming from the star, and this indeed allowed the detection of multiple interesting molecules on these far-off worlds, for example: carbon monoxide, carbon dioxide, water, hydrogen, methane and more. In the future the detection of “biomarkers”—evidence of extraterrestrial life—will be attempted using this technique.

The observed global temperature map of exoplanet HD 189733 b, the first of its kind, as inferred from the different phases of this remarkable hot Jupiter. Temperatures range from about 650 degrees Celsius on the coldest part, to 930 degrees Celsius on the hottest. Note that this hottest spot on the planet is not directly in the middle, i.e. it is not just
The observed global temperature map of exoplanet HD 189733 b, the first of its kind, as inferred from the different phases of this remarkable hot Jupiter. Temperatures range from about 650 degrees Celsius on the coldest part, to 930 degrees Celsius on the hottest. Note that this hottest spot on the planet is not directly in the middle, i.e. it is not just “below” the star or at “high noon”—but rather shifted to the East.

Moreover, by observing these planets at longer wavelengths, in the infrared, one can observe light emitted from the planet (vs. just reflected from—or refracted by—it) and thus permit us to measure the planet’s temperature on the day side. Some planets also allow the creation of rudimentary temperature maps (!) for them, finding that the hottest point on the day-side of the planet is not exactly facing the star—but shifted from it by strong, persistent jet streams. At that point one can start talking about the planet’s energy budget and global weather patterns, cloud formation and circulation,… characterizing the planet, and not just detecting it.

In some other cases “transit timing variations” were identified: the transits of some pairs of planets are not quite periodic but they appear to transit slightly earlier or later than they “should”, and in sync; when one was late, the other was early. These perturbations are cause by the gravitational interaction between different planets in the systems: both are pulling on each other, disturbing their regular rhythms. This allows us to reverse the problem and ask: “if I do see these irregularities, what kind of masses can cause them?”, the answer effectively finds the mass of the planet(s) in the system without ever using the expensive resources like HARPS—but for free—just by carefully analyzing the times of transit.

By studying yet finer details of the transit light curve—some of which have been detected and some are still too difficult to find even with current space-based data—many more things can be inferred about the planet: from planetary rings, from planetary oblateness to a measure of its rigidity, to planetary rotation rate and mean wind speed—all are derivable (in principle) from transit light curves.

We are thus able to sometimes measure the size, density, composition, dynamical interaction and much more for transiting planets, and I remind you: all that for a planet we can’t resolve or even directly see, and only because by some pure chance they happen to cross the face of their host star as seen from Earth.

P1330163 crop

About the author. Aviv Ofir is a Dean’s Postdoctoral Fellow at the Weizmann Institute of Science’s Planetary Sciences department. Prior to arriving at Weizmann, he was a Minerva Postdoctoral Fellow at Göttingen University in Germany. He has been a member of the science team of the HATNet ground-based transit survey, as well as the space-based CoRoT and Kepler transit surveys and the Cool Tiny Beats radial velocity collaboration. Dr. Ofir has extensive experience analyzing large photometric datasets, and invented a number of techniques for the efficient detection of faint signals in these data.

Las estrellas ¡laten!

Por Cristina Rodríguez-López, Instituto de Astrofísica de Andalucía

¿Perdón? ¿Las estrellas qué? ¡Sí, las estrellas “laten”! ¡Incluso nuestro Sol! Se suele pensar que las estrellas están allá arriba en el firmamento, inmóviles, quemando su combustible nuclear de forma confortable y silenciosa, pero la realidad que hemos descubierto a través de su observación es bastante diferente. Las estrellas “respiran”, se “contorsionan” y “retuercen” de diversas formas, alterando su radio y temperatura superficial, lo que produce cambios periódicos en su luminosidad y velocidad en su superficie, que detectamos con nuestros telescopios e instrumentos. Estos efectos se conocen con el nombre técnico de pulsaciones, u oscilaciones, y la técnica que intenta extraer toda la información posbile de estas estrellas pulsantes se conoce como Astrosismología, o, en el caso específico de nuestro Sol, Heliosismología. La nomenclatura responde a las técnicas utilizadas, análogas a las de la sismología terrestre, que extraen informacion de las ondas sísmicas propagándose en el interior de nuestro planeta para derivar la composición y estratificación de la Tierra. La Astrosismología analiza las frecuencias de oscilación de la luz procedente de las estrellas, que son la huella dactilar de la composición química y estructura del interior estelar, así como de otros parámetros físicos fundamentales, como su masa, densidad y edad.

Entonces, ¿qué son estas pulsaciones? Las pulsaciones son, estrictamente hablando, ondas de presión y gravedad (normalmente llamadas modos p- y g-) que se propagan en el interior de la estrella; se pueden pensar como ondas sonoras y marítimas, respectivamente, es decir, provocadas por cambios de presión y flotabilidad. Los modos p- y g- se propagan a diferente profundidad en el interior de la estrella (ver Figura 1), permitiendo sondear las diferentes regiones, que de otra forma serían inaccesibles, con sólo medir su frecuencia en la superficie.

Figura 1. Vista esquemática de dos modos de pulsación diferentes propagándose en el interior de una estrella. Los modos p- son menos profundos y se reflejan en la superficie estelar con mayor frecuencia que los modos g- que viajan más profundamente hasta el interior estelar. Crédito: Tosaka – Own work, CC BY-SA 3.0,

 El hecho de que algunas de estas oscilaciones sean ondas acústicas es la razón por la cual, poéticamente, se suele hablar de “la música de las estrellas”. Las ondas acústicas resuenan en el interior estelar de la misma forma que en un instrumento musical, y aunque sus frecuencias son demasiado bajas para que nosotros, los humanos, podamos oirlas -y porque el sonido no se propaga en el vacío-, algunos científicos las han amplificado, para que seamos capaces de escuchar como suenan. Sin embargo, la experiencia no es la más placentera del mundo, ya que las ondas acústicas en una estrella no son armónicas.

¿Pero cómo se originan las pulsaciones? Las pulsaciones se originan por el desplazamiento del plasma en el interior de la estrella. La radiación producida en los procesos de fusión nuclear en el núcleo, o capas, de la estrella, busca alcanzar la superficie, pero al hacerlo, se encuentra algunas piedras en el camino: una son las llamadas zonas de ionización parcial de los elementos químicos. En estas capas, la opacidad de la estrella aumenta al aumentar la presión, bloqueando la radiación procedente del interior y empujando las capas superiores, que entonces se hacen más transparentes, liberando la radiación y cayendo de nuevo, para empezar el ciclo, como si fuese un proceso de inhalación-exhalación, de la misma forma en que funciona un motor. Si la excitación producida en estas regiones es mayor que el amortiguamiento producido en todas las demás, entonces muy probablemente la estrella mostrará oscilaciones en su superficie. Éste es el llamado mecanismo kappa y es el responsable de las pulsaciones en varios tipos de estrellas variables, tales como las RR Lyrae, delta Scutis, beta Cephei, subenanas calientes o enanas blancas. En estrellas que tienen una zona interior radiativa y una exterior convectiva, el flujo radiativo puede ser bloqueado y luego liberado en la interfase -o tacoclina- entre estas dos capas de forma cíclica, como es el caso de las variables gamma-Doradus. Finalmente, en estas estrellas parcialmente convectivas, como nuestro Sol, se pueden producir también oscilaciones estocásticas, debidas a los movimientos convectivos turbulentos en la superficie estelar -como sucede cuando calentamos agua en un recipiente-.

¿Todas las estrellas pulsan? Y Próxima, ¿es pulsante? ¡Buena pregunta! Para contestarla, podemos echar un vistazo al diagrama Hertzsprung-Russell pulsante (Figura 2) que sitúa todos los tipos de variables pulsantes conocidas en función de su temperatura y luminosidad. La línea discontinua diagonal que lo atraviesa contiene las estrellas en la secuencia principal (SP), que queman hidrógeno en el núcleo. Algunas de las delta-Scuti son estrellas pre-SP, mientras que gigantes como las Cefeidas o Mira, situadas sobre la SP, y subenanas y enanas blancas, como GW Vir, sdBV y DAV, por debajo de ella, son todas post-SP o estrellas evolucionadas. Así, parece que todas las estrellas, sin importar cuál sea su masa, temperatura o estado evolutivo, tienen el potencial de ser pulsantes; aunque hay que tener en cuenta que ¡no todas lo son! es decir, estas bandas de inestabilidad no son puras, sino que están pobladas también por estrellas “normales” no-pulsantes. En el caso de Próxima, y en general para enanas M, aún no sabemos si son pulsantes. Se han predicho las pulsaciones de forma teórica, pero aún no se han detectado observacionalmente, aunque ¡las estamos buscando! Sólo podemos estar seguros de que, si las oscilaciones existen, serán de muy baja amplitud, del orden de millonésimas de magnitud, si lo que monitoreamos es la luz que nos llega de ellas, o menos de 1m/s, si lo que medimos es cuánto sube y baja la superficie de la estrella debido a las oscilaciones. Si las oscilaciones tuviesen amplitudes superiores a estos límites, ya las habríamos detectado.

Figura 2. Diagrama Hertzsprung-Russell de pulsación. Las enanas M están localizadas en la parte inferior de la línea diagonal de secuencia principal, en color anaranjado-rojizo. Las ubicaciones de las diferentes clases de estrellas pulsantes están indicadas con elipses rayadas. Crédito:

Explícame entonces cómo se detectan las pulsaciones. Las frecuencias de oscilación, o inversamente, sus períodos, pueden variar desde sólo unos pocos minutos hasta horas o unos pocos días. Para enanas M, como Próxima, el rango de variación predicho más probable está entre unos 20 minutos y 3 horas. Para detectar estas oscilaciones usamos dos técnicas que también se utilizan en las búsquedas de exoplanetas: la fotometría y la espectroscopía. La fotometría mide la cantidad de luz procedente de una estrella durante un período de tiempo: si la estrella no es variable, su curva de luz, o luz recibida en función del tiempo, será constante; mientras que variará de forma periódica si es una estrella pulsante (ver Figura 3). La misma técnica es utilizada por misiones espaciales de satélites dedicados a la búsqueda de tránsitos planetarios, como KEPLER y CoRoT, y el futuro PLATO, que miden el disminución en el brillo de una estrella cuando un planeta que la orbita cruza nuestra línea de visión. La espectroscopía, a través del método de las velocidades radiales, mide los cambios periódicos en la velocidad de las líneas espectrales de la estrella, causados por la subida y bajada de la superficie estelar provocada por las oscilaciones; al igual que los cambios en la velocidad son producidos por el tirón gravitacional de un planeta orbitando la estrella; éste es el mismo tipo de observaciones que estamos llevando a cabo para Próxima con el espectrógrafo HARPS.

Figura 3. Curvas de luz de estrellas variables en el cúmulo M1. Credit:

Entonces, ¿qué papel juegan las pulsaciones en el descubrimiento de exoplanetas? En primer lugar, tenemos que estar seguros de que las pulsaciones no sean confundan con un planeta, ya que a veces, pueden imitarlo; además, si la estrella es pulsante, las observaciones en busca de planetas han de ser diseñadas para minimizar la influencia de las pulsaciones en la adquisición de datos, o corregir de ellas los datos a posteriori, antes de que se pueda evaluar la señal de un planeta. Sin embargo, lo más interesante es que cuando una estrella pulsante alberga un planeta, se puede derivar con mucha precisión la masa, radio y edad de la estrella, y ésta es una forma única y muy valiosa de determinar los parámetros físicos del planeta y su historia evolutiva. Así que, ¡ojalá encontremos muchos planetas en torno a estrellas pulsantes!


Sobre la autora. Cristina Rodríguez López es investigadora postdoctoral en el  Instituto de Astrofísica de Andalucía (CSIC, España) en el grupo de “Estrellas de baja masa y exoplanetas e instrumentación asociada”. Sus intereses científicos incluyen la astrosismología de estrellas de bajas masa en diferentes estados evolutivos y la búsqueda de exoplanetas. Previamente, recibió su doctorado por la Universidad de Vigo y fue investigadora postdoctoral en el Laboratorio de Astrofísica de Toulouse-Tarbes (hoy en día IRAP, Francia) e investigadora visitante en el Departamento de Física y Astronomía de la Universidad de Delaware (EEUU). Es reponsable del paquete científico “Astrosismología de estrellas enanas M” dentro del Consorcio CARMENES, que agrupa 11 instituciones españolas y alemanas en torno a la explotación científica del espectrógrafo CARMENES, un nuevo cazador de planetas enfocado al descubrimiento de planetas tipo Tierra en torno a estrellas M, el mismo objetivo perseguido por el proyecto Punto Pálido Rojo, del que también es co-investigadora y editora.

Finding life around our nearest neighbour

Ignas Snellen, Leiden Observatory, Leiden University, The Netherlands

How amazing would it be if we found that there exists a planet, with a mass and temperature just like Earth, around our nearest neighbour—Proxima Centauri. How could we find out whether life exists on such a world?

The  Pale Red Dot project is all about following up a hint that such a planet may exist. This is extremely exciting. Finding such a planet may actually not be such a surprise. Proxima is a faint red dwarf star, seven times smaller than the Sun. From previous observations, for example using the NASA Kepler satellite targeting planets that transit their host star, it is clear that in general red dwarf stars indeed often have small rocky planets. Therefore, Proxima—our nearest neighbour at a distance of 4.2 light-years—could be expected to also host small planets. Since the luminosity of Proxima is one thousand times smaller than that of the Sun, the energy a planet receives from Proxima is that same amount less than it would receive from the Sun. Therefore a planet in an Earth-like orbit would be freezing cold. Astronomers like to think that to host life a planet needs to be able to sustain liquid water. It is crucial for life as we know it as a solvent; making the complex chemical reactions associated with biological activity possible. Indeed, no life on Earth can function without liquid water. For planets around Proxima it means that their orbital distances need to be significantly smaller, only a fraction of the Earth-Sun distance, to be able to sustain life—corresponding to an orbital period of about two weeks, right in the ballpark of the possible planet chased by Pale Red Dot.

Artist's impression of a habitable planet around a red dwarf star (credit ESO/L. Calçada).
Artist’s impression of a habitable planet around a red dwarf star (credit ESO/L. Calçada).

Let us for now assume that the Pale Red Dot observations indeed reveal such a planet. How could we possibly find out there is life on it? Let me first sketch the picture of why this is so difficult. For hundreds of years astronomers have wondered whether there is life on Mars, without a conclusion yet.  Over the last fifty years, Mars research has accelerated at an immense pace. NASA and ESA have sent many probes that dig, drill, and can measure the Mars atmospheric constituencies to high precision—and still we do not know. One has to realize that we will never be able to do this for extrasolar planets. The distances are simply too large. Even Proxima, our nearest neighbour star, is more than two-hundred-thousand times further away than Mars. We simply cannot send probes to Proxima on practical human time scales. Therefore, any information we collect from possible planets orbiting Proxima can only come from remote sensing—observing them using our telescopes on and around Earth.

Is it then entirely hopeless that we could find life? Luckily not! Of course, if the situation is like on Mars, where life may be hiding deep under the surface, or on Jupiter’s moon Europa, where simple life may be deep in its ocean, it will indeed be hopeless. We will never be able to recognize it from a distance. However, the situation is very different for Earth. If an alien civilization would point a telescope at Earth and measure its spectrum, it can see clear signs of biological activity. They can see that molecular oxygen is very abundant in our atmosphere, which is only present due to the organisms that produce oxygen as a waste product (which subsequently animals like us use as an energy source). Oxygen is a very reactive gas, which you do not expect to find in an atmosphere like ours. Indeed it took life on Earth more than a billion years before the oceans were saturated enough that the oxygen they produced ended up in the atmosphere. If all life on Earth would cease to exist, all atmospheric oxygen would disappear on a very short time-scale. Therefore we call oxygen a biomarker gas—it can provide evidence for biological activity on an Earth-like planet. Note however that a lack of oxygen does not mean there is no life. It could still hide under a rock like possibly on Mars.

Also, for more than a billion years there was abundant life on Earth without a significant amount of oxygen in the atmosphere. Anyway, at least we can start somewhere.

So how could we detect oxygen on a planet more than four light years away? Characterizing a planetary atmosphere is significantly more difficult than finding the planet, like is being tried now with the Pale Red Dot project. Most of the techniques used to find planets, including the radial velocity method used for Proxima, are indirect methods. They do not identify one single photon from the planet, but instead indirectly infer the presence of a planet—e.g. using the gravitational pull of the planet on the host star, or the moment a planet transits the disk of its host star blocking a small fraction of starlight that can be observed. This can no longer be the case for atmospheric characterization. We really need to identify photons from the planet as a function of wavelength, and in this way build up a planet spectrum. Although this is very difficult, this can be done, but is so far almost exclusively achieved for hot gas giant planets.

Bird's eye view of ESO's Very Large Telescope which is used for many of the exoplanet characterisation observations (credit: ESO).
Bird’s eye view of ESO’s Very Large Telescope which is used for many exoplanet characterisation observations (credit: J.L. Dauvergne & G. Huedepohl (

Broadly speaking, separating the planet’s light from that of the star can be done in the time, spatial, spectral and polarization domain, or using combinations of these. An example of the time domain is transmission spectroscopy. When a planet, as seen from Earth, moves in front of its host star, a little bit of starlight filters through the planet’s atmosphere, leaving an imprint of absorption from its atmospheric constituencies. A planet can also be eclipsed by its host star, temporarily blocking the planet light, which can be measured. In such a way the thermal emission spectrum or reflected light spectrum can be determined. However, such transit and eclipse observations require that the planet orbit is seen exactly edge-on – which will only be a small probability for the alleged Proxima planet. We have a better chance by trying to separate the planet from the star in the spatial domain. This is called direct imaging, or high-contrast imaging. Using a combination of techniques the starlight can be suppressed by orders of magnitude, leaving the planet signal coming from a slightly different direction unaffected.

Spectrometers coupled with very high contrast imagers on giant telescopes should enable the separation of the light coming from the star and the planet. In this picture, a simulation of the distinct orbital velocity of the planet and the star would allow to achieve higher contrast than using direct imaging alone. Source : Snellen et al. A&A 2015, arXiV
Spectrometers coupled with very high contrast imagers on giant telescopes should enable the separation of the light coming from the star and the planet. In this picture, a simulation of the distinct orbital velocity of the planet and the star would allow us to achieve higher contrast than using direct imaging alone. The signal of the planet image is the faintest dot on the right of the top panel. Source : Snellen et al. A&A 2015, more information in

Although Proxima is our nearest neighbour, the targeted planet’s orbit will be very close in—only ~1/200,000th of a degree (20 milli-arcseconds) as seen from Earth. The sharpness of a telescope directly scales with its diameter, implying that revealing a planet at such a small angular distance from its host star requires a mirror diameter of at least 25 meters. Even the James Webb Space Telescope, which will be launched in 2018, will not be able to separate this planet from its host star. We would really have to wait until the next generations of ground-based telescopes come online, like the US Thirty Meter Telescope and Giant Magellan Telescope, and the European Extremely Large Telescope. Even with these giants it will be a real challenge—we will have to look through our own atmosphere to detect the atmosphere of the planet. However, we have been practicing just that using giant planets over the last decade, and we are starting to get pretty good at it! We will have to be patient though—do not expect the specific instrumentation needed to detect oxygen to be ready before 2030. A long wait, but the prospects are very exciting!


About the Author: Ignas Snellen is Professor in astronomy at the University of Leiden in the Netherlands. After concluding his PhD research in Leiden in 1997, he worked for three years as a postdoctoral fellow at the Institute of Astronomy in Cambridge (UK), after which he became an astronomy lecturer at the University of Edinburgh (UK). He returned to Leiden University in 2004. Snellen and his group develop observation and data-reduction techniques for ground-based telescopes, particularly geared to be used for the future extremely large telescopes (ELT). He and his group pioneered studies of molecules in exoplanet atmospheres using high resolution spectroscopy in the near infrared.

Primera mitad de las medidas Doppler

Ahora que hemos relizado la mitad de las observaciones previstas con HARPS, y ASH2, nos gustaría compartir con vosotros el aspecto de los datos Doppler. Como vimos en el artículo ‘La señal’, esperamos una cierta variabilidad de ‘algunos’ metros por segundo, pero no más de 4-5 m/s, sino, el programa de búsqueda realizado por UVES ya la habría encontrado.

Desafortunadamente, no podemos revelar los datos reales para evitar sesgos en la futura evaluación del manuscrito. En lugar de ello, os presentamos unos cuantos ejemplos de medidas Doppler similares a las que estamos obteniendo para Proxima Centauri. Son simulaciones de datos obtenidos usando los mismos datos temporales que los de la campaña Punto Rojo Pálido y reproducen los tres resultados más probables que se pueden obtener de estas primeras treinta medidas. Pero le hemos dado una vuelta de tuerca! Uno de los seis conjuntos de datos se corresponde, de hecho, con las observaciones ‘reales’… ¿podéis averiguar cuál es?

Caso 1 –  Variabilidad en la velocidad radial dominada por ruido aleatorio

Figura 1 – Los paneles de la izquierda muestran dos conjuntos de posibles medidas Doppler; los paneles centrales muestran una de las herramientas utilizadas para detectar posibles periodicidades y los de la derecha muestran los mejores ajustes a los datos al ponerlos en fase con los períodos más favorables obtenidos en los paneles centrales. No encontramos ninguna variabilidad suficientemente significativa en ninguno de los dos conjuntos de datos. Créditos : Guillem Anglada-Escude/

Los paneles de la izquierda en la Figura 1 muestras dos ejemplos típicos de datos que sólo contienen ruido aleatorio. Las pequeñas líneas verticales de cada punto son las llamadas barras de error, e ilustran la incertidumbre de cada medida (~1 m/s). Hay que tener en cuenta que dependiendo de las condiciones atmosféricas, algunas medidas tienen mayores barras de error. Los paneles centrales muestran un gráfico llamado periodograma. Los periodogramas nos dicen cuáles son los períodos más significativos posibles en los datos y nos permiten cuantificar si una señal es o no lo suficientemente robusta como para se detectada.  En este ejemplo fijamos el umbral de detección a una probabilidad de falsa alarma del 0.1%. Es decir, los picos que sobrepasen la línea discontinua azul corresponderían a señales con probabilidad de falsa alarma menor que el 0.1%. Ninguno de estos dos conjuntos de datos revela una señal significativa.

Caso 2 – Indicios de una señal, pero alterada por la actividad

Figura 2 – Una inspección a ojo sugiere que podría haber variabilidad coherente, pero no puede distinguirse del ruido estelar. Los ajustes Keplerianos de la derecha no son muy buenos y requieren ajustes orbitales con excentricidades muy altas, lo que es característico de variabilidad espuria. Créditos : Guillem Anglada-Escude/

Aquí mostramos dos conjuntos de datos que contienen una posible señal Doppler, pero que han sido alterados por actividad estelar no periódica. Como en el caso 1, ninguno de los dos conjuntos de datos son suficientes para confirmar una señal. La acumulación de datos a lo largo de la campaña, debería impulsar los verdaderos candidatos a planetas sobre los límites de detección, al mismo tiempo que la significancia de las señales espurias disminuiría. En casos como éstos, intentaríamos modelar la actividad estelar utilizando fotometría y otras medidas espectroscópicas, para ver si parte de la variabilidad puede ser explicada por ruido estelar. Como ejemplo de las técnicas utilizadas para conseguir esto, podéis consultar la entrevista a la catedrática Suzanne Aigrain.

Caso 3 – Se detecta una señal con claridad, a pesar de la actividad

Figure 3 - In this two cases, signals stands out over the threshold and the right fits look a bit better, Note that these sets only contain 1/2 of the data and are barely above threshold, so even in this case we would need to wait until the end of the run and the photometric monitoring to see if their significance improves. Image credits : Guillem Anglada-Escude/
Figura 3 – En estos dos casos, señales Doppler significativas destacan sobre el umbral de detección. Créditos : Guillem Anglada-Escude/

En este caso tenemos dos conjuntos de datos simulados con señales auténticas de planetas que dominan claramente sobre el ruido (Figura 3). Este sería el mejor escenario para la campaña Punto Rojo Pálido. Aún así, tendríamos que investigar la fotometría y otros índices de actividad para evaluar la posible variabilidad relacionada con la actividad.

¡Gracias por seguirnos!


— Traducido del inglés por Cristina Rodríguez López–

Why we are all metal-heads!!

By James Jenkins, Universidad de Chile

Here on planet Earth, we all know what metals are. They are the components of the man-made industrial world around us. From the aluminium tins that contain our fizzy drinks, to the copper cables that distribute power across the globe, all the way up to the giant iron building structures that dominate our city skylines.   However for astronomers, metals are something quite different. They are the atoms that were not created in any great abundance in the Big Bang[1]. This basically means that astronomers call all atoms metals, except Hydrogen and Helium. All these atoms that were previously processed in the hearts of giant stars, or in the intense stellar explosions called Supernova, and continue to be so today. Carl Sagan’s thoughts on metals were poetically portrayed in his famous quote that appeared in the book Cosmos: “The nitrogen in our DNA, the calcium in our teeth, the iron in our blood, the carbon in our apple pies, were made in the interiors of collapsing stars. We are made of starstuff.”

The abundance of metals, or metallicity, of objects throughout the universe, appears to have a considerable affect on the various properties of those objects. For instance, for Supernovae, the violent explosions that signify the deaths of massive stars, the metallicity of the progenitor star before it collapses to produce the explosion, plays a major role in the determination of what type of supernova the star will eventually become, and therefore, the amount of energy released in the explosion. However, in the exoplanet[2] community, the metallicity of stars took on a whole new meaning in 1997 after the first three exoplanet hosts were studied. It was found that all three of these stars had a much higher fraction of metals by mass in their atmospheres than the Sun does. They were found to be so called, metal-rich stars.

In the subsequent 19 years since this finding, astronomers have discovered that there is a direct correlation between the fraction of iron atoms in a star’s atmosphere and the probability of that star hosting a gas giant planet. In fact, it has been shown that for Sun-like stars with three times the metallicity of the Sun, around 30% have Jupiter-like giant planets orbiting them, whereas only 3% of stars with a mass similar to the Sun host these types of planets. This lower fraction of gas giant planet-hosting stars with lower metallicity continues down to stars with even lower fractions of metals by mass, whereby only 0.3% of stars with one-tenth the metallicity of the Sun host giant planets. This relationship was the first direct connection between the properties of stars that astronomers can measure observationally, and their retinue of planets.

It turns out that such a correlation as the one observed between gas giant planet fraction and stellar metallicity was a direct prediction of the core accretion planet formation process. At the time, the two competing formation channels for planets were core accretion and gravitational collapse. The core accretion formation process is a ‘bottom-up’ mechanism, where the smallest dust particles in the disc of material leftover from the formation of the star, begin to stick together, building up larger and larger pebbles, rocks, and finally planetesimals. The planetesimals can then go on and continue to grow, either by accreting more dusty material from the disc, or by sweeping up the disc’s reservoir of gas. On the other hand, the gravitation collapse channel is a ‘top-down’ mechanism, whereby the disc fragments into smaller pieces of dust and gas due to gravitationally unstable regions in the disc, and with continued collapse over time,  those pieces finally become giant planetary bodies orbiting the central star. In either case, it’s humbling to remember that planet Earth, where life clings to so voraciously, was born out of the stellar garbage left over after the mother Sun was born.

The percentage of stars hosting gas giant planets near to the host star with changing stellar metallicity ([Fe/H]). It can be seen that the stars with the most amount of metals in their atmospheres have a higher chance of growing a giant planet around them. The red curve shows the best-fit model to the data (coloured region) and the equation that describes the model is represented on plot. As discussed in the text, the percentage of stars hosting giant planets increases with the fraction of iron (Fe) over hydrogen (H) in a star’s atmosphere. Credit: Graphic modified from the original published by Fischer & Valenti 2005, ApJ.
Both these mechanisms make key testable predictions, and the fraction of gas giant planets orbiting stars as a function of metallicity was one that came to very different conclusions. Given that the core accretion model starts by sticking the smallest dust particles together to make larger structures, the more dust in the disc, the faster those structures can be built, and the faster those cores can acquire gas from the disc before the disc is lost to interstellar space. Given that the disc is leftover rubbish from the formation of the central star, discs rich in dust should also have formed stars rich in metals, or those with higher metallicities, seemingly in agreement with observations. On the other hand, the gravitational collapse model does not depend on the dust fraction in the disc and so less dusty discs should form as many large planets as dusty discs do, meaning no stellar metallicity bias should be witnessed. In the end, this was the key piece of evidence to suggest that planets are formed through a bottom-up process like core accretion.

With the recent advancement in technology in the laboratory, along with the latest data being fed to astronomers from orbiting space telescopes like Kepler, the picture may not be as clear cut for the population of lower-mass planets, particularly planets with masses similar to that of Neptune or less. It appears that the fraction of stars hosting these low-mass planets, aka. super-Earths, does not increase with increasing metallicity, in the same way as for giant planets. In fact, the opposite might be true, where low-mass planets tend to form predominantly around metal-poor stars.

An artists impression of a metal-rich planet forming disc around a young star. The star is the bright, illuminating source in the center of the disc, and small rocks and planetesimals are beginning to form around the star, due to the large amount of metals that can stick together and form these planet embryos. Credit: NASA/JPL

If the population of super-Earth planets do not follow the same pattern as giant planets, then what does this say about how these planets form? Does this mean they do not form through the same core accretion-type process as giant planets? Well the answer is no, it does not mean that. Remember that core accretion predicts that giant planets will be predominantly found orbiting metal-rich stars because the small cores that grow to become the large planetesimals that are needed to tear the gas away from disc must grow fast enough before the disc is lost. However, low-mass planets that are either core dominated or that don’t require significant amounts of gas have no need to form so quickly. In an environment where there is less metals, cores take longer to form, and therefore they maintain a small mass up until the disc is lost. Therefore, core accretion also predicts that low-mass planets should be more abundant orbiting metal-poor stars than gas giant planets, another win for the core accretion planet formation theory!!

Metallicity of planet host stars against the minimum mass[3] of the detected planets in those systems. Note that this is only for stars hosting planets with estimated masses in agreement with the mass of Neptune or less. The red shaded region is the super metal-rich part of the diagram and it appears to show a lack of planets when compared to the more metal-poor region in the left bottom quadrant of the plot. Credit: Graphic modified from our paper discussing this observational result.

The role that metals have played in the development of the evolving universe and for the emergence of life on planet Earth cannot be understated. Metals are the weaving that so intimately connects us all to the entire cosmos around us. Its ironic that such beauty emerges from such violent beginnings out there in space. As for Proxima Centauri, it is a super metal-rich star, meaning its small proto-planetary disc would have been rich in planet forming material. This at least gives us hope that some of those metals began the chaotic dance that ends with the birth of new planets, and who knows, with such a rich array of metals that could have been there in those early days, are there other life forms on those planets that have been fortunate enough to make use of the universe’s talent for metal production? Maybe the Pale Red Dot project will help us to find out!!


About the Author. James Jenkins is an assistant professor at the Universidad de Chile based in Santiago, the capital city of Chile. Nestled between the surrounding Andes mountain range atop Cerro Calan, he performs observations of nearby stars to hunt out and better understand extrasolar planets and their host stars. James received his Ph.D from the University of Hertfordshire in 2007, going on to hold a postdoctoral position at Pennsylvania State University, working on the Precision Radial Velocity Spectrograph. At the end of 2008 he found himself working at the Universidad de Chile as a postdoctoral researcher and then as a Fondecyt Fellow between 2010-2013, joining the faculty at the end of 2013. His main research interests include the discovery of planets orbiting metal-rich stars through the Calan-Hertfordshire Extrasolar Planet Search, the search for very low-mass planets in radial velocity data, and planets orbiting giant stars. For his sins, he also studies the magnetic activity of planet host stars, working to better understand how this source of ‘noise’ can be filtered out of planet search data. James is a very active member in the Pale Red Dot project and is one of the editors of


[1] The Big Bang is the name given to our current model for the moment of creation of the Universe.

[2] The word ‘exoplanet’ is the disminuative of the words ‘extra-solar planet’, worlds orbiting stars other than the Sun.

[3] Remember that the radial velocity detection method does not give the absolute mass of stellar companions, but instead gives us the ‘minimum mass’, since the inclination of the system to our line of sight is unknown.

Worlds of Rock and Ice

by Yiannis Tsapras, Zentrum für Astronomie in Heidelberg and

“The worlds are formed when atoms fall into the void and are entangled with one another; and from their motion as they increase in bulk arises the substance of the stars.” – Leucippus of Elea (5th century BCE)

What new knowledge may be gained by studying exoplanets? There is a direct syllogistic link between this fledgling field of inquiry and our progressive comprehension of the complex set of processes that we collectively define as life. Our understanding of life is derived from observations of its diverse manifestations on our home planet,  all of which are inextricably linked,  sharing a common biological origin – a single genesis. The discovery of a ‘second genesis’, of life elsewhere in the universe that does not rely on ribonucleic acid (RNA) and deoxyribonucleic acid (DNA),  has profound repercussions not only for science but for every field of human inquiry.  A top-down approach to addressing this issue directly is that of the Search for
ExtraTerrestrial Intelligence (SETI) project.  It began in the ’70s and has looked for signs of transmissions from alien civilizations ever since. An alternative approach involves a gradual exploration from the bottom-up, where new scientific knowledge may be gained with each intermediate step.

Planets form in gaseous disks surrounding young stars, but the exact physical processes that drive their formation and evolution are not yet fully understood.

We know that these disks last for a few million years and that planet embryos can migrate while they are still embedded in them. Some of these planetary embryos migrate into their host stars,  while others survive and grow throughout this process but end up far from where they first started forming.  How are these planets distributed around their host stars and are there similarities with our own system or is the Solar system in some ways unique? The presence of liquid water on a planet’s surface is not a guarantee for the existence of life,  but it is a necessary ingredient for the development of life as we know it.  Liquid water can only exist at a certain range of distances from the host star, thehabitable zoneWhat fraction of planets reside within the habitable zone of their host stars, are their orbits generally stable or unstable, and what are their physical characteristics? Finding these planets and examining their distribution is our first goal, both observationally and theoretically.  We seek to study their diversity and understand the processes that drive their formation and evolution.

Searches for extrasolar planets have already yielded such a bountiful, and extraordinarily diverse, harvest that it has been necessary to overhaul the planet formation model originally put forth to explain the Solar system. These discoveries include planets orbiting Pulsars, “Hot Jupiters“—gas giants that orbit their stars every few days, planets that have been ejected from their systems and are now floating alone in the darkness, and the first few Earth-sized planets orbiting far enough from their stars that any water on their surface would be in liquid form.

Astronomers use a variety of methods to find these planets and each method is sensitive to a different domain of the planet distribution.

The distribution of known exoplanets as a function of mass vs. semi-major axis (normalized to the location of the snow line). Planets discovered by radial velocity (black triangles), transits (red circles), direct imaging (blue squares), pulsar timing (yellow stars) and microlensing (green pentagons) are shown. The planets of the solar system (yellow circles) are also depicted for comparison. The region of sensitivity of each method is also indicated.
The distribution of known exoplanets as a function of mass vs. semi-major axis (normalized to the location of the snow line). Planets discovered by radial velocity (black triangles), transits
(red circles), direct imaging (blue squares), pulsar timing (yellow stars) and microlensing (green pentagons) are shown. The planets of the solar system (yellow circles) are also depicted for comparison. The region of sensitivity of each method is also indicated.

By studying the emerging patterns in this distribution, and testing the theoretical predictions with real data,  we develop our understanding of how planets form and how their orbits evolve. There is,  however,  a certain type of planet that we still know very little about; Cold rocky planets,  far enough from their stars that any water on their surface would have turned to ice. Theory predicts that at the early stages of planet formation,  proto-planetary embryos in this region are likely to form cores of ice and rock and,  provided the conditions are right, gradually grow by accreting material from the surrounding gaseous disk, transforming them into gas giant planets. However,  if there is little gas available,  or if it gets depleted quickly,  they do not grow very large. These planets are almost undetectable with transit or radial velocity searches, but are exactly the type of planet microlensing searches are designed to find.

Einstein predicted that any massive star will act as a gravitational lens,  bending the light rays from any background star that passes behind it,  as seen from the Earth,  and distorting its apparent shape. The effect of lensing at cosmological distances is practically observed as multiple distorted images of the background (source) star around the edge of the gravitational influence of the lensing star. In microlensing the angular distances between the images generated by the lensing effect are of the order of micro-arcseconds, and the images cannot be individually resolved with current technology.  What is actually observed during microlensing events is an increase in the brightness of the source star as the lens appears to move closer to it on the plane of the sky, followed by a gradual dimming back to its normal brightness as the lens moves away.

The relative proper motions between the stars in the Galaxy produce microlensing events that last for a few weeks up to several months. If the lens is a planetary system,  there is a chance that the planets may also perturb the light coming from the source star resulting in short-lived but intense anomalous features on the event lightcurve that reveal the presence of the planet. These anomalies typically last for a few days in the case of Jupiter-mass planets and only for a few hours for Earth-mass planets.  Since the presence of the lensing object can only be inferred by its gravitational effects and not the light it produces, the method can detect planets around stars that are extremely faint, even around brown dwarfs and black holes.

Lightcurve of microlensing event OGLE-2005-BLG-390 showing a 12-hour planetary anomaly attributed to a ~5.5 Earth-mass planet.
Lightcurve of microlensing event OGLE-2005-BLG-390 showing a 12-hour planetary anomaly attributed to a ~5.5 Earth-mass planet.

Microlensing is a rare phenomenon. In our own Galaxy, only about one in a million stars will undergo microlensing at any given time. Yet modern microlensing surveys (OGLE,  MOA), monitoring the
extremely crowded fields of the Galactic Bulge,  announce ~2,000 such events every year.  A small subset of these events is selected for monitoring by follow-up teams (RoboNet,  μFun,  MiNDSTeP, PLANET) and intensive observations commence to look for planetary deviations.

Early results from microlensing searches at intermediate orbital radii (1-10AU) indicate that ice and gas giant planets are a relatively common feature around M-dwarf stars. These searches have also found a number of quite massive planetary and brown dwarf companions orbiting low-mass stars, several planets with masses close to that of the Earth, systems with multiple planets, and possible first evidence of an exomoon. Over the next few years, ground-based searches will be complemented by space missions, which will allow for a much clearer understanding of the planet distribution at and beyond the icy regions of planetary systems.


About the Author. Currently holding a research position at the Zentrum für Astronomie in Heidelberg,  Yiannis previously sated his scientific curiosity working for the LCOGT institute (2007-2014). During the 2012-2014 academic period he was also a Teaching Fellow at the School of Physics and Astronomy, Queen Mary University where he taught Physics for the Science and Engineering Foundation Programme and a MSc course on Extrasolar Planets and Astrophysical Discs. Prior to that, he held a research position at the ARI in Liverpool. He received a PhD in Astronomy from the University of St Andrews in 2003 and a MSc in Radioastronomy from the University of Manchester in 1999.  His  primary research interests lie in the field of exoplanet science where he uses the complementary techniques of microlensing and transits to search for planets orbiting distant stars. He is a founding member of the RoboNet project which uses the LCOGT telescope network to detect exo-planets by microlensing. Besides exoplanets, he has a keen interest in robotic astronomy, ongoing dark-matter surveys, CMB cosmology and science outreach programs.

Exciting times, big challenges

By Luca Pasquini, European Southern Observatory

What incredible times we are living in — searching for an Earth around another star! Not much more than 20 years ago, I looked at the few astronomers hunting for planets, and I shook my head and thought “they are crazy”. Similar to many other occasions throughout my life, I was to be proven wrong.

Nature, of course, helped those early planet hunters quite a lot, by making Hot Jupiters. These are systems inducing radial velocity variations 10 times larger, and with much shorter periods, than the giant planets of the Solar System, which were the only ones known at that time. I believe that the influence of the discovery of the first confirmed exoplanet 51 Pegasi b by Mayor and Queloz, will be very long lasting indeed. By proving the existence of what was before then only considered likely to some of us, or an obvious hypothesis for others, their work unleashed a wealth of energy to the subject that had been unthinkable before. We are now able to analyse exoplanet atmospheres, and to search for small mass exoplanets in the habitable zones of other stars, planets that can harbour life in the way we know it.

Such a tremendous explosion of results has only been possible because fundamental technological advancements have taken place in the past 20 years, advancements that now allow us to search for solar systems and Earth analogues.

Previous expert opinions have shown us that, in order to detect the planetary radial velocity signals, a lot of effort is needed to filter the stellar ‘noise’ (activity, oscillation, variability), and in order to best do that, one needs very precise spectroscopy and long observing campaigns. This requires proper instrumentation and dedicated telescopes. Several observatories such as the European Southern Observatory (ESO) are well equipped with both.

A HARPS Laser Frequency Comb generated spectrum. The horizontal lines are spectral orders (each has two separated fibres, one fed by starlight, the other by A frequency comb combs). The colour reflects the covered spectral range, from short wavelengths (blue) to long ones (red). Each horizontal line corresponds to a diffraction order and is generated and it is composed of thousands of separated, single emission peaks, whose frequency is known with very high accuracy, and are stable over long times. LFC are the next generation of ‘rulers’ to measure precise radial velocities.
A HARPS Laser Frequency Comb generated spectrum. The horizontal lines are spectral orders (each has two separated fibres, one fed by starlight, the other by A frequency comb combs). The colour reflects the covered spectral range, from short wavelengths (blue) to long ones (red). Each horizontal line corresponds to a diffraction order and is generated and it is composed of thousands of separated, single emission peaks, whose frequency is known with very high accuracy, and are stable over long times. LFC are the next generation of ‘rulers’ to measure precise radial velocities.

Precision is the key word. The radial velocity signal induced by an Earth orbiting around a solar mass star with a period of 1 year, is less than 10 cm s-1. Just to provide some comparison, this implies that we must be able to measure the periodic shift of the stellar radial velocity in the focal plane of a typical high-resolution spectrograph for several orbital periods, over several years with a peak shift of just 2 nanometers (10-9 meters or 0.000000001 meters). In addition to requiring the utmost care in stabilising the instruments in temperature and pressure, reaching such a precision requires a very precise ruler, and for this reason several groups in the world have been engaged for almost a decade in work developing the perfect ruler. Currently the most precise rulers are based on Laser Frequency Combs (LFCs), a technique that led to the Nobel Prize for physics being awarded to T. Hänsch and J. Hall in 2005. The LFC can create a series of precisely equally spaced and stable emission lines for spectrograph calibration, whose frequency is known with high accuracy. The worldwide leader instrument in radial velocity precision is probably HARPS at ESO’s La Silla Observatory in Chile. Up to now it has been using the emission line Thorium-Argon lamps as a ruler, but it has been recently equipped with a prototype Laser Frequency Comb system. The short-term tests of this system indicate that a precision of better than 2 cm s-1 can be reached. Advances in understanding optical fibres and their technology, and getting bigger and better optical detectors have also been vital in obtaining the best performance. Optical CCDs are now very clean devices that can be accurately calibrated.

The Laser Frequency Comb hardware in the HARPS room at the ESO 3.6m telescope at La Silla, it is 'a bit' more complex system than a lamp.
The Laser Frequency Comb hardware in the HARPS room at the ESO 3.6m telescope at La Silla, it is ‘a bit’ more complex system than a lamp.

Great expectations are placed on ESPRESSO, the ‘big brother’ instrument to HARPS, that will be hosted at the ESO Very Large Telescope at Paranal before the end of the year. This instrument will boost the original HARPS precision by one order of magnitude and, in addition, will be used by any of the VLT telescopes, or by the four 8-metre Unit Telescopes together, with a 16 metre telescope equivalent diameter. Often the stars observed are relatively bright, so one could question why large telescopes are needed, but we must realise that high precision requires also a lot of stellar photons, or particles of light, hence the quest for large telescopes. A further step in precision is expected from the high-resolution spectrograph at the 39-meter E-ELT. The CODEX concept was originally conceived to measure Doppler shifts so precise such that we would be able to directly observe the expansion of the Universe and Earth-like planets around solar type stars in their habitable zones. The 25-metre Giant Magellan Telescope is planned to have a similar instrument for its first light.

The ESPRESSO CCD. With 81 million pixels, this device is the largest monolithic detector ever used in astronomy. Each side is 9 cm long.

Planets are cool compared to stars, and emit most of their light as infrared (IR) radiation, which is invisible to the human eye. Expanding observations to this spectral range is therefore essential, and the development of large IR detectors played a fundamental role: progressing in a few years from arrays of a few thousand pixels, to the most recent 16 million pixel devices, which enabled the construction of efficient high resolution infrared (IR) spectrographs. These spectrographs, such as CRIRES at the VLT, have been used to hunt for planets and to observe exoplanet atmospheres. In addition, the radial velocity signal produced by the rotation of inhomogeneities on the stellar surface can mimic the RV periodic variations induced by a planet, but , while the variations induced by the planet are the same for any measured wavelength of light, they are different in the optical and in the IR for the stellar spots that rotate around the star’s surface. That is why the newest generation of spectrographs have a great interest in the IR, and NIRPS, which will be hosted at the ESO 3.6-metre telescope at La Silla, CARMENES at the Calar Alto Observatory, Spirou at CHFT, and the high resolution spectrograph for the E-ELT, will all have an IR arm.

Even if this contribution focuses on radial velocities and spectroscopy, we should not underestimate the power of imaging. NACO at the VLT has imaged the first exoplanet around a very low mass star, similar to Proxima Centauri, and it is beyond any doubt that images, like the one shown below, have been transformational. More powerful high contrast imagers recently became available, imagers such as SPHERE at the VLT and GPI at GEMINI. These create superb images of planets and proto-planetary discs and are able to detect objects more than one million times fainter than the host star. And the next generation of instruments that will be able to exploit the tremendous potential of the ELTs is already taking shape.

The NACO image of an exoplanet (red dot) close to a very low, cool mass star. Possibly the first image of an exoplanet ever. Credits: ESO
The NACO image of an exoplanet (red dot) close to a very low, cool mass star. Possibly the first image of an exoplanet ever. Credits: ESO

Large surveys are now carried out and images of exoplanets are becoming more and more common. The enabling technology has been adaptive optics, a technique that deforms mirrors to compensate for the atmospheric turbulence and therefore recovers the cleanest image of the telescope, as if it was in space, observing with no turbulent atmosphere to look through. Deformable mirrors with more than 1000 actuators, applying corrections faster than 1000 times per second are needed, and they have been developed either of small size, for instance for SPHERE and GPI, or of large size, and these are directly replacing the secondary mirrors of the telescopes, as has happened at the Large Binocular Telescope and soon will occur at the VLT.

The Adaptive Secondary Mirror of the VLT is 1.12 m in diameter and extremely thin: the glass shell is only 2 mm thick. Being so thin, it can be easily deformed, and 1170 actuators act on the back of the glass to correct in real time the distortions induced by the Earth's atmosphere in the observed images.
The Adaptive Secondary Mirror of the VLT is 1.12 m in diameter and extremely thin: the glass shell is only 2 mm thick. Being so thin, it can be easily deformed, and 1170 actuators act on the back of the glass to correct in real time the distortions induced by the Earth’s atmosphere in the observed images.

In a nutshell, thanks to all these great instruments, exoplanet science has a bright present, and even more promising future.


lucaAbout the author. Luca Pasquini is an astronomer, working at ESO, Garching, and since 2013 he has been managing the Paranal Instrumentation Programme. After completing his studies in Firenze (Italy), he moved to become an ESA postdoc at MPE (Germany) in 1986, and then went on to ESO La Silla (Chile), where he was in charge of high resolution spectroscopy and of the 3.6m telescope upgrade. In 1997 he moved to ESO Garching, to work in the instrumentation group there. Before his present position, he has been instrument scientist for the FEROS, HARPS, FLAMES, MUSE, and ESPRESSO spectrographs. His scientific work and interests range from stellar activity and stellar abundances, to search for planets around giant stars and around stars in open clusters, as well as to different applications of precision spectroscopy.