Saturday, January 28, 2017

The HST 'bacon' program: PanCET

What is PanCET?

PanCET is the largest exoplanet observation program ever to be run with the Hubble Space Telescope. Now, PanCET stands for the Panchromatic Comparative Exoplanet Treasury and is a program which consists of 498 HST orbits (that is 32 solid days of Hubble time), and over twice the size of any Hubble exoplanet program that has come before it. The aim of the program is to measure the atmospheres of 20 exoplanets, over 3 instruments, in 6 different modes, as they are eclipsed by or transit their stars.

So let me take you through each part of the name to explain where it comes from.

Pan for Panchromatic.

Panchromatic means that we are looking at the atmospheres of these planets over many colors or more accurately wavelengths. This program will combine observations from the UV through the optical and out into the near-infra red. This type of investigation is important to get a complete picture of what the atmosphere of these planets is made of. The UV looks for evidence of Hydrogen escape high in the atmosphere, where some planets appear more like comets with their atmospheres streaming off behind them as they orbit their stars. Observations in the optical take you deeper into the atmosphere to look for sodium and potassium absorption, or evidence of scattering by clouds. And the near-infrared expands this investigation to find evidence of water vapor in the atmosphere which can tell us about the abundance of oxygen. So with panchromatic observations we can probe the Hydrogen oxygen and even in cases the carbon chemistry of the atmospheres from the top to the bottom.

Diagram of irradiated exoplanet atmospheric structure, illustrating which atmospheric layers are affected by different irradiation wavelengths. The plots from Lavvas et al. (2014) show the temperature (left) and abundance of major species (right) vs pressure. Taken directly from the PanCET proposal (credit: D. Sing, M. Lopez-Morales).  
C is for Comparative.

So, we have a nice wide wavelength range but the next part of the name is key, comparative. This program is looking at 20 different exoplanets, from hot jupiters which will be mostly hydrogen and helium, to Neptune and sub-neptune sized worlds where we know little about the composition of the atmosphere and the dynamics of the atmosphere. A number of the planets in the program have been observed before so PanCET is filling in the wavelength gaps and where a planet may have been observed in the optical we are now making observations in the UV and Near-IR, or where a planet is observed in the near-ir we are getting the optical data for it. This wide range of targets and observations allows us to make detailed comparisons between all of the planets and their atmospheric spectra to try and understand how they are similar or different to look for trends in their parameters.

E is for Exoplanet.
Figure from Sing et al. (Nature, 2016).
Showing the HST transmission spectra of 10 transiting
exoplanets. PanCET will expand this list to over 25
exoplanets with complete wavelength coverage.
So we have a PANchromatic Comparative and I am hoping E for exoplanet is self explanetory. The last part is then "Treasury".

T is for Treasury.

This part is a directive from HST to the scientific community and is defined as follows:
"The goal of these programs is to increase the scientific impact of HST, in part by providing sets of high-level science products to the astronomical community that are useful for addressing multiple scientific topics." 
In each HST cycle just over 1000 orbits of HST are awarded to treasury programs so PanCET was not only deemed big for exoplanet science, but science as a whole with nearly half of the total time available. Transiting exoplanets are an amazing resource of information and will be the leading force behind exoplanet discovery and understanding for decades to come and PanCET is just the sprinting start.

Finally, the PIs that lead the program are Drs David Sing from the University of Exeter and Mercedes Lopez-Morales from Harvard University. I spoke to Dr Sing earlier and he said
“I’m very humbled and exited at the opportunity to use of the greatest scientific instruments of all time to look in-depth and explore a whole diverse zoo of planets.”
But importantly PanCET also means bacon in Italian so it is really the Hubble bacon program - bringing in the bacon for exoplanet studies everywhere!

PanCET is for everyone.

While the team assembled by the PIs will be leading the analysis efforts and working on putting the whole thing together, the data and products made by the team will be available to the whole community. So go explore, investigate, and discovery. Then share what you have learned.

What's next?

That is up to you and me; each year there is a call sent out for the community to propose to the Hubble Space Telescope and ask what it is we want it to scientifically investigate. As I said this is only the sprinting start of a marathon of exoplanet studies. We need to put forward our ideas and discover what is out there, how planets form, what planets are made of, and how does our little blue dot fit into the grand universe of alien worlds.

Links to the PanCET proposal can be found here:
Links to the HST call for proposals can be found here:
The deadline is Friday, April 7, 2017, 8:00 pm EDT.

And any questions you have about PanCET and its selected instruments, wavelengths, or planets can be asked below. 

Wednesday, July 20, 2016

Double transit all the way across the star!

Artist impression of the TRAPPIST-1b and -1c transit.
Credit: NASA, ESA, and G. Bacon (STScI) with
science credit to NASA, ESA, and J. de Wit (MIT)
On May the 4th the Hubble Space Telescope (HST) trained its mirror on a little ultra-cool dwarf star, just 39-light years away, called TRAPPIST-1. What it saw was a rare, and before unseen event, two Earth-sized exoplanets passing in front of the star just minutes apart. These two planets, TRAPPIST-1b and TRAPPIST-1c, were discovered by a Belgian robotic telescope at ESO's La Silla Observatory in Chile. The TRAnsiting Planets and PlanetesImals Small Telescope (TRAPPIST) telescope has only just begun it's search of the 1,000 nearest dwarf stars and came up with a winner.

There are a lot of papers and press articles you can read on this which I will link at the bottom, but here I wanted to tell my story of involvement and why I think this is a great step forward in exoplanet science.

One thing to note is that TRAPPIST-1, the star, is just 2,500K that is cooler than some exoplanets that have been discovered. This means that even though it's planets b and c are very close with orbits of just 1.5 and 2.4 days respectively, they are still relatively temperate with estimated temperatures of around 250 degrees - similar to the inner planet of our solar system. The first thing that needs to be worked out to take our understanding of the implications further is what is the atmosphere made up of? This is a key step towards understanding these worlds and the nature of their environments.
"What I love most about these observations is the presence of both planets distinctly transiting the star just minutes apart. "
On May the 4th a team led by Julien de Wit from Massachusetts Institute of Technology (MIT) used Hubble to observe the system to get an idea of this. A week earlier I was called while in the UK by Nikole Lewis, who was leading the team from Space Telescope Science Institute (STScI), who asked if I would be interested in analyzing some new data she was involved with from Hubble for small earth sized planets. I was not told much more about what I would be analyzing or the nature of the observations but loving HST analysis and trusting Nikole I agreed. The day I flew back to The States, I remember landing and reading my Twitter feed to see that there had been a Nature paper on the discovery of three Earth-sized planets around a dwarf star. I then immediately emailed Nikole to ask if these were the planets we would be analyzing with Hubble. A day before the observations were to be taken I was called and told I should come up to STScI, just and hour north of Washington DC in Baltimore, to work on the data with the team as they would be getting access to it early in the morning. So I headed up for the start of what turned out to be an intense week or so of back a forth analysis and paper writing. As the only outsider to the TRAPPIST team, called in specifically to apply my expertise on analyzing Hubble exoplanet data I spent some time playing catch up, but quickly realized what a fantastic opportunity this was and how special these planets may be. So I want to say a massive thank you to the TRAPPIST team and Nikole for inviting me in, and for being so welcoming since.

What I love most about these observations is the presence of both planets distinctly transiting the star just minutes apart. You can see that in the light curve in our paper. First TRAPPIST-1c (red), the outer planet, starts to transit, then just 12 minutes later TRAPPIST-1b (green) starts to transit. Due to the size/speed of their orbits they both then pass out of the disk of the star relative to us, the observer, at the same time. The blue model shows the effect of the combined light blocked out by both of the planets during the course of the observations.

You can see in the video as part of the STScI press release an artist impression of this configuration.
Fig 1 of the Nature paper - I have modified it by removing the top panel for the purpose of this blog post.
See the paper for the full figure and caption. 

For these observations we used Wide Field Camera 3 (WFC3) on Hubble to observe this event in the near-infrared, just beyond the red part of what our eyes can detect. At these wavelengths you can detect the absorption from different things in the atmosphere by seeing how the amount of light blocked by the planets changes with small changes in the wavelength/color. This method is called transmission spectroscopy and has been used to look at the atmospheres of many exoplanets (see my previous blog post on #HJSurvey).
"I see great things for the future of exoplanet studies by looking at the TRAPPIST-1 system, and I look forward to seeing or even working on more results from the team."
The observations we took of both TRAPPIST-1b and -1c showed us that these small Earth-sized worlds do not have large envelopes of hydrogen and helium. This is great! The lack of a puffy atmosphere like that of the gas giants in our solar system further hints at the rocky, terrestrial nature of these worlds. What you can see here is the measurements we made across the different wavelengths (black points), compared to different model atmospheres. Due to the combined signal of the two planets we were able to get very precise measurements, considering they are such small worlds around a small star. This is the first step towards future measurements of both planets as they transit the star apart over the next few years to rule out and confirm different atmospheric compositions.
Fig 3 of the Nature paper - This shows the transmission spectra of TRAPPIST-1b and TRAPPIST-1c compared to different atmospheric models. The top is the combined transit measurements, the bottom shows the measurements made by deconstructing the light curve into the two planet components. 

With more Hubble observations we could potentially detect water in the atmosphere and get an idea of the depth of the atmosphere, or we could even get an idea if the planet has methane in its atmosphere. These types of preliminary observations are vital in the lead up to the launch of the James Webb Space Telescope (JWST) in 2018, which will be the next great observatory in space. JWST will get us even more information across more wavelengths where perhaps even biosignatures like CO and Ozone can be detected. We will also attempt to get more precise information on the planets temperatures and even possible the surface pressure.

Another important aspect of these observations is the star itself. We actually know very little about M-stars. The classification of TRAPPIST-1 is M8 which means it is a very small very cold star. In fact it is so cold (in relative terms) it has a significant amount of water vapor that can exist in the stars atmosphere. One of the things we had to do for these observations was enlist the expertise of Jeff Valenti at STScI to help understand how the light from the star itself will change at different wavelengths so that it could be accounted for in each of our wavelength bins. There is still so little we know about the impact an M-star will have on the atmospheres or even habitability of their planets that this is another reason why looking at these systems is so fascinating. We need to study more M-star systems to get a better idea of their stars and understand how they change the planets that form and evolve.

Small planets around small stars - where the relative amount of light being blocked out in transit then becomes large - are key steps towards our understanding of habitability, formation, and atmospheric dynamics. I see great things for the future of exoplanet studies by looking at the TRAPPIST-1 system and I look forward to seeing or even working on more results from the team.

The NATURE paper can be found on arXiv or on the Nature website for those with a subscription.

The original discovery paper of the TRAPPIST-1 system

Here is the link to the official HST press release
NASA press release

Related articles for this press release can be found here
MIT EAPS press release
National Geographic
Guardian UK Science

NASA Snapchat story active from July 20th 1pm - 21st 1pm

NASA Goddard press video


Sunday, January 31, 2016

My exoplanet memories

This is what I was doing in 1995.
Conducting, Counting, and at the beach. These weirdly follow my
real life. But those trousers in the middle, what were they thinking.
It is strange, when I think about the discovery of exoplanets, I cannot place the first time when it dawned on me they were real and not just science fiction. When I give talks about exoplanets to young audiences I am always quick to point out that they are the first generations to grow up always knowing that other worlds outside of our solar system exist. But, I fear I have been lying to myself this whole time, and I am actually part of that generation too. 

In 1995 when exoplanets hit the big time, with the discovery of 51 Pegasi b, I was 5/6 years old. I was in year 1/2 at school (kindergarten/1st grade). My memories of that time are limited. I was modeling for children book publisher DK, where my aunt and uncle worked, and dreaming of becoming a farmer with my friends at school where we would have a farm to look after sick animals. The only science fiction we had been introduced to at this time by my mother was Quantum Leap, and Stargate was not due to be made into a TV show for another two years. 

All I recall from the years following 1995 is my interest changed from farm animals to dinosaurs, spurred on by the 1993 release of Jurassic Park, and Jurassic park lost world in 1997. As this was all accompanied by trips to the Natural History Museum in London with the school, and clear memories of my friend being terrified of the animatronic T-Rex ripping apart another dinosaur as I walked past grinning and loving it. 

We were not introduced to Star Trek or Star Wars growing up, because our mother did not watch it so we didn’t.The first experience of epic science fiction journeys to other worlds came in the form of Stargate SG1. When Stargate, a pivotal information source of my future ambitions and endeavors, did reach my consciousness we were already adventurers and explorers. My parents enrolled us in a snorkeling club where we went on big trips to the lake or the coast to explore the world under the waves. My father a amateur historian loved to take us to castles, towns, and museums. By the early 2000’s we were all planning to be Egyptian archeologists or marine biologists.

It was not until 2001/2 that I distinctly remember turning towards space*. My Father used to drive me to the Guildford astronomical society evenings, to listen to talks or look through a real telescope. Every single year our family grabs some bin liners and goes out to the field out the back of the house to lie down and look up at the sky during the Perseid meteor shower, but I don’t remember when that started, it is just something we have always done but quite honestly could be a relatively new tradition. 

*In 2002 the first atmospheric detection was made of a transiting exoplanet (Charbonneau et al. 2002), work which forms the basis for what I do now as a postdoc. 

Samantha Carter (Amanda Tapping)
from Stargate SG1. We had this photo
signed on our bedroom wall for at least
7 years. Then I took it with me to put
on  my wall at Uni.
Since I decided I wanted to be a real life Samantha Carter (Stargate Astrophysicist, adventurer, and all round depended on kick ass woman), I have not turned back. But by then the presence of other alien worlds as the norm was in my head, the new Star Wars prequels were out, we were having lightsaber fights in the science classroom with the meter rulers, and I was going to sic-fi conventions to meet people from Stargate, Lord of the rings, the matrix, and a host of other shows featured in SFX each month. 

When I went to university exoplanets were not yet part of the general curriculum for undergrad classes. I selected my university degree based on how much space I could learn about, and by how far away they could send me for a year. I ended up at the University of Wales: Aberystwyth, the most awkward to get to from my parents home, where they sent me to Svalbard in the Arctic to finish up my MPhys year. It is half way through my time at Aberystwyth that I remember openly talking about exoplanets as a real scientific discovery. We were asked to write an essay about water on Mars or other planets. As we were enrolled in a Planetary and Space Physics degree, most of us had worked on Venus or Martian data, so I remember most of the class writing about that. But, I wrote an essay on exoplanets and the plans for the upcoming Kepler mission to find all of these strange new alien worlds, of course I linked it all back to Stargate in some way. I loved the work I did on the solar system planets, and the impact the Sun’s atmosphere had on our inner solar system, but I knew I wanted to work on exoplanets. I wanted to find an Abydos, or Chulak. I wanted to discover what they were like, was it anything we had seen before. Did Stargate get any of it right?

In 2010 myself and a friend convinced our advisor to apply to the Royal Astronomical Society for a summer internship position at the university to search through the first sets of data coming from the Kepler Exoplanet Mission. To link it to our work on the Sun, where we had previously been looking at CME tracking and sunspot evolutions, my friend used the Kepler data as a search for starspots to model their influence on the light curve, while I set about looking for planets transiting them. 

I had my taste of what being an exoplanet explorer could be and I wanted to keep doing it as long as I could get away with it. But looking back there was no eureka moment. No point in time where I sat there and thought, ‘holy shit they are real and people have just discovered them’. They were always just there, be it in science fiction which I did not know was not based on truth yet, or in reality. As my earliest memories of the world stem from a time when they actually did exist despite the fact I was born in a world where they did not, I cannot truly claim to be part of the last generation to grow up with this world changing discovery. 

But I think I am okay with that. Now I am part of the first generation to grow up always knowing we were not a lone solar system drifting at the reaches of our galaxy. Like Pluto I have been reborn.

Me talking about exoplanets, and comparing hot Jupiters to a watermelon.

Monday, December 14, 2015

Clear to Cloudy

As of this morning the NASA Exoplanet archive lists the discovery of 1916 exoplanets. These planets range in size and mass all the way from super Jupiters (over 10 times the mass of Jupiter), to Neptune’s, super-Earths (up to 10 times the mass of the Earth), and potentially Mars-sized or even Mercury-sized worlds. One of the most interesting discoveries in the search for exoplanets is that many of them are nothing like what we have in our solar system.

One such class of planet that was discovered is the hot Jupiter. Hot Jupiters are similar to Jupiter in mass , but can range in size from 0.8 - 2 times as large in their radius. Hot Jupiters also orbit much closer to their host stars than Jupiter in our own solar system, which sits at a cool 5 time the distance from the sun as the Earth, in fact hot Jupiters orbit 20 times closer to their star than we do to the Sun, which is even closer than even Mercury. This means that they are also tidally locked, with one face of their planet in constant daylight and the other in constant night.  

But now the new and exciting stuff...

To get an idea about what these strange new alien worlds are like, an international team of astronomers harnessed the observing power of the Hubble space telescope, and the Spitzer space telescope to conduct the most extensive study thus far to characterise the atmospheres of ten hot Jupiters. By looking at the stars light as the planet transits in front of the star, as Venus does in our solar system, from the perspective of the Earth we can detect the unique fingerprints of different molecules in the planets upper atmosphere as the light is filtered through before reaching our telescopes. This measurement of how the atmosphere absorbed light at different wavelengths is called transmission spectroscopy.

HST/Spitzer transmission spectral sequence
of hot Jupiter survey targets.
The solid lines are the model spectra fit to the measured transmission
spectra of each hot Jupiter in the survey, which are shown as data
points with their measured uncertainties. The spectra are offset and ordered
from top to bottom with low to high values of 
In the past only a small number of well-studied planets (HD 209458b, HD189733b, GJ 1214b) have been analyzed over a small wavelength range between 1.1-1.7 microns, just beyond the red part our eyes can see (Deming et al. 2013; Line et al. 2013; Sing et al. 2014; McCullough et al. 2014; Sing et al. 2015). This is an important wavelength range as it is where water vapor absorbs sunlight. Recent studies have shown that hot Jupiters have much smaller and muted water features than is predicted. The smaller signals could potentially be explained by lower amounts of water than was expected (Seager et al. 2005; Madhusudhan et al. 2014), which is a sign that water is removed somehow from the protoplanetary disk from which a solar system would form (Oberg, Murray-Clay, & Bergin 2011), but it is not clear if this high level of depletion is even possible. Alternatively, the weak signals of water vapor could be the result of clouds or hazes in the hot Jupiters atmosphere which obscure the water signals (Pont et al. 2013; Sing et al. 2014, 2015; Nikolov et al. 2015)

This new study published in Nature shows the measurements of ten hot Jupiter atmospheres from the optical (0.3 microns) all the way out into the mid-infrared (5 microns). This allows us to spectral resolve not only the water feature in the near-IR, but also the optical scattering and the IR molecular absorption features. The result of the study reveal a diverse group of planetary environments from clear atmospheres, which exhibit little to no evidence for high altitude clouds or hazes, revealing broad atomic signatures in the optical to large amplitude water features in the IR, to cloudy and hazy planets, which have strong Rayleigh scattering slopes in the optical and muted or even absent absorption features from water in the IR.

Pressure-Temperature profiles and condensation curves.P-T profiles were calculated from 1D radiative transfer
models (Fortney et al. 2008). Condensation curves are calculated for
chemical species expected in hot Jupiter atmospheres (Morley et al. 2012).
The presence of a cloud or haze can be predicted by the atmospheres temperature profile with altitude. Models show that as we move higher and higher in the planets atmosphere, decreasing log(pressure), the temperature decreases. Where the temperature and pressure of the atmosphere match the temperature and pressure where a material will change from a gas to a liquid is called the condensation point (Wakeford et al 2015). This will form the base of the cloud in that atmosphere. This is shown in the figure where the colored lines cross the grey dashed lines. Yet strangely the presence of obscuring clouds and hazes in the observations do not match up perfectly with the predictions from the models. So temperature and pressure alone cannot explain the clear to clouds atmospheres observed, suggesting circulation, vertical mixing need to be considered to transport heat and particles around the planet (Showman & Polvani 2011).

In the study we present a metric to distinguish between planetary atmosphere, comparing the difference between the measured planetary radius in the near-IR to that measured in the mid-IR (ΔZJ-LM), and correlate this with the strength (amplitude) of the water absorption feature. We additionally define the difference between the optical and mid-IR (ΔZUM-LM) that compares the strength of scattering in the optical, to the molecular absorption measured by Spitzer.

Transmission spectral index diagram: ΔZJ-LM vs H2O amplitude.The uncertainties represent the 1-sigma uncertainty. The purple and grey lines show model 
trends for cloudy and hazy atmospheres. We also show the clear-atom models with sub-solar
abundances in red. Note: WASP-39b and WASP-6b are missing as they currently have no
HST/WFC3 data. However, we have both scheduled for this coming year.
By plotting our measurements from this broad wavelength study we show that the results favor the obscuration of water by clouds or hazes rather than models where the water abundance is lower. The effect of clouds or hazes in the atmosphere reduces the water absorption amplitude, while raising the level of the near-IR to mid-IR continuum levels, leading to high ΔZJ-LM with low water amplitudes.

Theoretical model transmission spectra.
Model spectra assuming 1200K temperature with gravity of 25 m/s^2.
Models in each panel are compared to a clear, solar metallicity atmo (black).
This has revealed a continuum of hot Jupiter atmospheres from clear to cloudy. With the cloud formation in the atmospheres of these planets being highly sensitive to the temperature and pressure profile such steep gradients in the upper atmospheres, mean changes of just 100 degrees either way can totally change the cloud properties being observed. You can also see the different models that go with these metrics below.

This is the first time a large comparative study has been conducted on exoplantary atmospheres using consistent analysis techniques to combine datasets from different instruments and spacecraft. It is fantastic to finally see them all together in one place so that we can start to unravel the mysteries of these planets from afar.

The exciting part is now with this metric we can attempt to classify such strange alien planets, and the James Webb Space Telescope, Hubble’s successor, will expand our range of planets to study even further. Importantly, with more and more observations we may be able to make our own solar system planets part of this interstellar comparison. 

You can find the full nature paper on the Nature site here 

Also check out all of the press releases on the survey below