Giving my invited talk on how planets affect cool stars at the Cool Stars 20 conference.
This summer the Cambridge Workshop on Cool Stars, Stellar Systems and the Sun had its 20th anniversary, and took place in Boston. This is my favourite conference series, and this year I was really excited because I had the honour of being an invited speaker. I gave a talk on “How planets affect cool stars”, and had a lot of good interactions with people about the science of stars and exoplanets. This was the first time I’ve given an invited talk wearing a “My little pony” T-shirt. Also, this was the first time for me to introduce my PhD students to the Cool Stars community, which was a neat thing I hadn’t had the chance to do before.
It was a fantastic meeting, with lots of scientific input, and it was wonderful to see all my friends and colleagues from the Harvard-Smithsonian Center for Astrophysics again.
Part of the X-ray emission line spectra of AB Dor A and alpha Cen B analyzed in this study (Wood et al. 2018).We investigated the X-ray emission line spectra of cool main-sequence stars in order to construct their emission measure distributions and compare them to the Sun:
“A Chandra/LETGS Survey of Main-sequence Stars”
We analyze the X-ray spectra of 19 main-sequence stars observed by Chandra using its LETGS configuration. Emission measure (EM) distributions are computed based on emission line measurements, an analysis that also yields evaluations of coronal abundances. The use of newer atomic physics data results in significant changes compared to past published analyses. The stellar EM distributions correlate with surface X-ray flux (FX) in a predictable way, regardless of spectral type. Thus, we provide EM distributions as a function of FX, which can be used to estimate the EM distribution of any main-sequence star with a measured broadband X-ray luminosity. Comparisons are made with solar EM distributions, both full-disk distributions and spatially resolved ones from active regions (ARs), flares, and the quiet Sun. For moderately active stars, the slopes and magnitudes of the EM distributions are in excellent agreement with those of solar ARs for logT< 6.6, suggesting that such stars have surfaces completely filled with solar-like ARs. A stellar surface covered with solar X-class flares yields a reasonable approximation for the EM distributions of the most active stars. Unlike the EM distributions, coronal abundances are strongly dependent on spectral type, and we provide relations with surface temperature for both relative and absolute abundances. Finally, the coronal abundances of the exoplanet host star τ Boo A (F7 V) are anomalous, and we propose that this is due to the presence of the exoplanet.
A Chandra/LETGS Survey of Main-sequence Stars, Wood, Brian E.; Laming, J. Martin; Warren, Harry P.; Poppenhaeger, Katja, The Astrophysical Journal, Volume 862, Issue 1, article id. 66, 24 pp. (2018).
I was invited to give a talk on “How Stars and Planets Interact: a Look Through the High-Energy Window” at the XMM-Newton 2018 Science Workshop with a focus on X-ray time-domain astronomy. As always, had some very nice interactions with the colleagues at ESAC in Madrid. It’s interesting to hear what’s new in all the other subfields being probed by soft X-rays.
New paper: Unmasking a hot Jupiter in an unresolved binary system ?>
The NGTS planet-search project in which I take part has detected a new planet in an interesting system:
Transit light curve of the newly discovered Hot Jupiter NGTS-3Ab, from Günther et al. (2018).
“Unmasking the hidden NGTS-3Ab: a hot Jupiter in an unresolved binary system”
We present the discovery of NGTS-3Ab, a hot Jupiter found transiting the primary star of an unresolved binary system. We develop a joint analysis of multi-colour photometry, centroids, radial velocity (RV) cross-correlation function (CCF) profiles and their bisector inverse slopes (BIS) to disentangle this three-body system. Data from the Next Generation Transit Survey (NGTS), SPECULOOS and HARPS are analysed and modelled with our new BLENDFITTER software. We find that the binary consists of NGTS-3A (G6V-dwarf) and NGTS-3B (K1V-dwarf) at <1" separation. NGTS-3Ab orbits every 1.675 days. The planet radius and mass are Rplanet=1.48 ± 0.37 RJand Mplanet=2.38 ± 0.26 MJ, suggesting it is potentially inflated. We emphasise that only combining all the information from multi-colour photometry, centroids and RV CCF profiles can resolve systems like NGTS-3. Such systems cannot be disentangled from single-colour photometry and RV measurements alone. Importantly, the presence of a BIS correlation indicates a blend scenario, but is not sufficient to determine which star is orbited by the third body. Moreover, even if no BIS correlation is detected, a blend scenario cannot be ruled out without further information. The choice of methodology for calculating the BIS can influence the measured significance of its correlation. The presented findings are crucial to consider for wide-field transit surveys, which require wide CCD pixels (>5″) and are prone to contamination by blended objects. With TESS on the horizon, it is pivotal for the candidate vetting to incorporate all available follow-up information from multi-colour photometry and RV CCF profiles.
Unmasking the hidden NGTS-3Ab: a hot Jupiter in an unresolved binary system, Günther, Maximilian N.; Queloz, Didier; Gillen, Edward; Delrez, Laetitia; Bouchy, François; McCormac, James; Smalley, Barry; Almleaky, Yaseen; Armstrong, David J.; Bayliss, Daniel; Burdanov, Artem; Burleigh, Matthew; Cabrera, Juan; Casewell, Sarah L.; Cooke, Benjamin F.; Csizmadia, Szilárd; Ducrot, Elsa; Eigmüller, Philipp; Erikson, Anders; Gänsicke, Boris T.; Gibson, Neale P.; Gillon, Michaël; Goad, Michael R.; Jehin, Emmanuël; Jenkins, James S.; Louden, Tom; Moyano, Maximiliano; Murray, Catriona; Pollacco, Don; Poppenhaeger, Katja; Rauer, Heike; Raynard, Liam; Smith, Alexis M. S.; Sohy, Sandrine; Thompson, Samantha J.; Udry, Stéphane; Watson, Christopher A.; West, Richard G.; Wheatley, Peter J., accepted for publication by Monthly Notices of the Royal Astronomical Society, 2018.
Locations of the telescopes that are part of the KOINet project (from von Essen et al. 2018).I am happy to be part of the Kepler Object of Interest Network, a network of ground-based telescopes to observe transits of exoplanets discovered by the Kepler space telescope in order to figure out their masses through Transit Timing Variations.
The first paper about this project is now accepted:
“Kepler Object of Interest Network I. First results combining ground and space-based observations of Kepler systems with transit timing variations”
During its four years of photometric observations, the Kepler space telescope detected thousands of exoplanets and exoplanet candidates. One of Kepler’s greatest heritages has been the confirmation and characterization of hundreds of multi-planet systems via Transit Timing Variations (TTVs). However, there are many interesting candidate systems displaying TTVs on such long time scales that the existing Kepler observations are of insufficient length to confirm and characterize them by means of this technique. To continue with Kepler’s unique work we have organized the “Kepler Object of Interest Network” (KOINet). The goals of KOINet are, among others, to complete the TTV curves of systems where Kepler did not cover the interaction timescales well. KOINet has been operational since March, 2014. Here we show some promising first results obtained from analyzing seven primary transits of KOI-0410.01, KOI-0525.01, KOI-0760.01, and KOI-0902.01 in addition to Kepler data, acquired during the first and second observing seasons of KOINet. While carefully choosing the targets we set demanding constraints about timing precision (at least 1 minute) and photometric precision (as good as 1 part per thousand) that were achieved by means of our observing strategies and data analysis techniques. For KOI-0410.01, new transit data revealed a turn-over of its TTVs. We carried out an in-depth study of the system, that is identified in the NASA’s Data Validation Report as false positive. Among others, we investigated a gravitationally-bound hierarchical triple star system, and a planet-star system. While the simultaneous transit fitting of ground and space-based data allowed for a planet solution, we could not fully reject the three-star scenario. New data, already scheduled in the upcoming 2018 observing season, will set tighter constraints on the nature of the system.
“Kepler Object of Interest Network I. First results combining ground and space-based observations of Kepler systems with transit timing variations”, von Essen, C.; Ofir, A.; Dreizler, S.; Agol, E.; Freudenthal, J.; Hernandez, J.; Wedemeyer, S.; Parkash, V.; Deeg, H. J.; Hoyer, S.; Morris, B. M.; Becker, A. C.; Sun, L.; Gu, S. H.; Herrero, E.; Tal-Or, L.; Poppenhaeger, K.; Mallonn, M.; Albrecht, S.; Khalafinejad, S.; Boumis, P.; Delgado-Correal, C.; Fabrycky, D. C.; Janulis, R.; Lalitha, S.; Liakos, A.; Mikolaitis, S.; Moyano D’Angelo, M. L.; Sokov, E.; Pakstiene, E.; Popov, A.; Krushinsky, V.; Ribas, I.; Rodriguez S., M. M.; Rusov, S.; Sokova, I.; Tautvaisiene, G.; Wang, X., accepted by Astronomy & Astrophysics, 2018.
New paper on the Star Formation Region Serpens South ?>
Spitzer infrared false-colour image of the Serpens South field. Protostars are shown in red, as is the cool dust that permeates the region. Shocked gas is visible in green, and the dust lane shows in black. The white dashed boxes indicate the approximate monitored fields.As part of the Young Stellar Object VARiability project (YSOVAR), I am happy to report that we have published a new paper investigating the mid-infrared variability of young stellar objects in the star-forming region Serpens South. Here’s the title and abstract:
“YSOVAR: Mid-infrared Variability among YSOs in the Star Formation Region Serpens South”
We present a time-variability study of young stellar objects (YSOs) in the Serpens South cluster performed at 3.6 and 4.5 μm with the Spitzer Space Telescope; this study is part of the Young Stellar Object VARiability project. We have collected light curves for more than 1500 sources, including 85 cluster members, over 38 days. This includes 44 class I sources, 19 sources with flat spectral energy distributions (SEDs), 17 class II sources, and five diskless YSO candidates. We find a high variability fraction among embedded cluster members of ∼70%, whereas young stars without a detectable disk display no variability. We detect periodic variability for 32 sources with periods primarily in the range of 0.2–14 days and a subset of fast rotators thought to be field binaries. The timescale for brightness changes are shortest for stars with the most photospheric SEDs and longest for those with flat or rising SEDs. While most variable YSOs become redder when fainter, as would be expected from variable extinction, about 10% get bluer as they get fainter. One source, SSTYSV J183006.13‑020108.0, exhibits “cyclical” color changes.
“YSOVAR: Mid-infrared Variability among YSOs in the Star Formation Region Serpens South”, Wolk, Scott J.; Günther, H. Moritz; Poppenhaeger, Katja; Winston, E.; Rebull, L. M.; Stauffer, J. R.; Gutermuth, R. A.; Cody, A. M.; Hillenbrand, L. A.; Plavchan, P.; Covey, K. R.; Song, Inseok, The Astronomical Journal, Volume 155, Issue 2, article id. 99, 20 pp. (2018).
New paper: X-ray line coincidence photopumping in a solar flare ?>
Energy level diagram for the transitions involved in this X-ray photopumping mechanism. This is actually the first time that one of my papers has an energy level diagram plot in it.This is somewhat unusual research for me, but it was good fun – some recent work about identifying an emission line in the X-ray regime which is excited by photons from a different atomic species which just happens to have the correct wavelength for that. This can be used as an independent density diagnostics for plasma in flaring loops, for example. The paper has just been published, here is the title and abstract:
“X-ray line coincidence photopumping in a solar flare”
Line coincidence photopumping is a process where the electrons of an atomic or molecular species are radiatively excited through the absorption of line emission from another species at a coincident wavelength. There are many instances of line coincidence photopumping in astrophysical sources at optical and ultraviolet wavelengths, with the most famous example being Bowen fluorescence (pumping of O III 303.80 Å by He II), but none to our knowledge in X-rays. However, here we report on a scheme where a He-like line of Ne IX at 11.000 Å is photopumped by He-like Na X at 11.003 Å, which predicts significant intensity enhancement in the Ne IX 82.76 Å transition under physical conditions found in solar flare plasmas. A comparison of our theoretical models with published X-ray observations of a solar flare obtained during a rocket flight provides evidence for line enhancement, with the measured degree of enhancement being consistent with that expected from theory, a truly surprising result. Observations of this enhancement during flares on stars other than the Sun would provide a powerful new diagnostic tool for determining the sizes of flare loops in these distant, spatially unresolved, astronomical sources.
“X-ray line coincidence photopumping in a solar flare”, Keenan, F. P.; Poppenhaeger, K.; Mathioudakis, M.; Rose, S. J.; Flowerdew, J.; Hynes, D.; Christian, D. J.; Nilsen, J.; Johnson, W. R., Monthly Notices of the Royal Astronomical Society, Volume 474, Issue 3, p.3782-3786, 2018.
New paper and press release: Discovery of a monster planet ?>
Artist’s impression of planet NGTS-1b with its neighbouring star (credit University of Warwick/Mark Garlick).A timely discovery for Halloween: Our NGTS collaboration has discovered a “monster planet”, a giant planet around a very small star. This is very surprising, because barely any of those huge planets have been found close to tiny stars. We will have to re-think some of our planet formation theories.
And here is the scientific information from the paper: We present the discovery of NGTS-1b, a hot-Jupiter transiting an early M-dwarf host in a P=2.674d orbit discovered as part of the Next Generation Transit Survey (NGTS). The planet has a mass of 0.812 Mjup, making it the most massive planet ever discovered transiting an M-dwarf. The radius of the planet is 1.33 Rjup. Since the transit is grazing, we determine this radius by modelling the data and placing a prior on the density from the population of known gas giant planets. NGTS-1b is the third transiting giant planet found around an M-dwarf, reinforcing the notion that close-in gas giants can form and migrate similar to the known population of hot Jupiters around solar type stars. The host star shows no signs of activity, and the kinematics hint at the star being from the thick disk population. With a deep (2.5%) transit around a K=11.9 host, NGTS-1b will be a strong candidate to probe giant planet composition around M-dwarfs via JWST transmission spectroscopy.
“NGTS-1b: A hot Jupiter transiting an M-dwarf”, Bayliss, Daniel; Gillen, Edward; Eigmuller, Philipp; McCormac, James; Alexander, Richard D.; Armstrong, David J.; Booth, Rachel S.; Bouchy, Francois; Burleigh, Matthew R.; Cabrera, Juan; Casewell, Sarah L.; Chaushev, Alexander; Chazelas, Bruno; Csizmadia, Szilard; Erikson, Anders; Faedi, Francesca; Foxell, Emma; Gansicke, Boris T.; Goad, Michael R.; Grange, Andrew; Gunther, Maximilian N.; Hodgkin, Simon T.; Jackman, James; Jenkins, James S.; Lambert, Gregory; Louden, Tom; Metrailler, Lionel; Moyano, Maximiliano; Pollacco, Don; Poppenhaeger, Katja; Queloz, Didier; Raddi, Roberto; Rauer, Heike; Raynard, Liam; Smith, Alexis M. S.; Soto, Maritza; Thompson, Andrew P. G.; Titz-Weider, Ruth; Udry, Stephane; Walker, Simon. R.; Watson, Christopher A.; West, Richard G.; Wheatley, Peter J.; accepted for publication by Monthly Notices of the Royal Astronomical Society (2017).
The twelve 20 cm telescopes of the NGTS facility at Cerro Paranal, Chile (Wheatley et al. 2017).The mission paper about the Next Generation Transit Survey (NGTS), a ground-based telescope network to search for transiting exoplanets, has just been published. I’m happy to be part of this project, which is a collaboration between several universities in the UK, Germany, Chile, and Switzerland – lots of exciting discoveries to come soon!
Here’s some more info about the paper: We describe the Next Generation Transit Survey (NGTS), which is a ground-based project searching for transiting exoplanets orbiting bright stars. NGTS builds on the legacy of previous surveys, most notably WASP, and is designed to achieve higher photometric precision and hence find smaller planets than have previously been detected from the ground. It also operates in red light, maximising sensitivity to late K and early M dwarf stars. The survey specifications call for photometric precision of 0.1 per cent in red light over an instantaneous field of view of 100 square degrees, enabling the detection of Neptune-sized exoplanets around Sun-like stars and super-Earths around M dwarfs. The survey is carried out with a purpose-built facility at Cerro Paranal, Chile, which is the premier site of the European Southern Observatory (ESO). An array of twelve 20cm f/2.8 telescopes fitted with back-illuminated deep-depletion CCD cameras are used to survey fields intensively at intermediate Galactic latitudes. The instrument is also ideally suited to ground-based photometric follow-up of exoplanet candidates from space telescopes such as TESS, Gaia and PLATO. We present observations that combine precise autoguiding and the superb observing conditions at Paranal to provide routine photometric precision of 0.1 per cent in 1 hour for stars with I-band magnitudes brighter than 13. We describe the instrument and data analysis methods as well as the status of the survey, which achieved first light in 2015 and began full survey operations in 2016. NGTS data will be made publicly available through the ESO archive.
“The Next Generation Transit Survey (NGTS)”, Wheatley, Peter J.; West, Richard G.; Goad, Michael R.; Jenkins, James S.; Pollacco, Don L.; Queloz, Didier; Rauer, Heike; Udry, Stephane; Watson, Christopher A.; Chazelas, Bruno; Eigmuller, Philipp; Lambert, Gregory; Genolet, Ludovic; McCormac, James; Walker, Simon; Armstrong, David J.; Bayliss, Daniel; Bento, Joao; Bouchy, Francois; Burleigh, Matthew R.; Cabrera, Juan; Casewell, Sarah L.; Chaushev, Alexander; Chote, Paul; Csizmadia, Szilard; Erikson, Anders; Faedi, Francesca; Foxell, Emma; Gansicke, Boris T.; Gillen, Edward; Grange, Andrew; Gunther, Maximilian N.; Hodgkin, Simon T.; Jackman, James; Jordan, Andres; Louden, Tom; Metrailler, Lionel; Moyano, Maximiliano; Nielsen, Louise D.; Osborn, Hugh P.; Poppenhaeger, Katja; Raddi, Roberto; Raynard, Liam; Smith, Alexis M. S.; Soto, Maritza; Titz-Weider, Ruth; accepted for publication by Monthly Notices of the Royal Astronomical Society (2017).
Musings on scientific discoveries, luck, and being prepared ?>
I’ve been thinking about the relationship between luck and good preparation lately. We have published a paper on the discovery of three plus one small planets around a small star recently, and we basically did the work for that in one day. The way that worked out got me thinking.
From the outside, what happened was this: Data from the latest Kepler-K2 campaign was publicly released. My student Rob Wells looked through some light curves and found something that looked like a triple-planet system. We started writing a paper about it, and had it finished after a bit more than one day of full-steam-ahead work. We submitted it to the journal (MNRAS Letters), and the arXiv, in the early evening. Got some helpful and thorough comments from the reviewer, edited the paper draft, got it accepted, done. From the outside, I imagine that this looks like being quite lucky.
From the inside of our group, there was actually much more work involved. My student had spent a lot of time over the past half year to get a data crunching pipeline working, which did quite a number of things (detrending the telescope data, doing a rough search for transits fully automatically, producing image files that allow the human user to quickly browse through stuff and sort for things that look like interesting systems). I had previously worked on spectral energy distributions of stars for another project (the YSOVAR project and my paper in the project series), and had some experience with proper MCMC fitting of transits from yet another project (my work on X-ray transits). All this preparation meant that we could directly jump into the relevant analysis for the paper and write it up with a collaborative online latex editor really quickly. We had to determine the stellar spectral type, produce proper transit fits (which eventually revealed the fourth planet candidate), and perform a stability analysis for the spectrum (in which our colleague Chris already had some experience, so he got that up and running really quickly). A lot of this came down to having all of the necessary experience in our small team. It would have been even better if we had all of the necessary tools and code somewhere easily accessible in one place – that’s what we have done now with a shared code repository for our group, so that other discoveries should be publishable quite quickly from now on. I’m really happy about this.
Another thing I like about how all of this worked out: My student came to me with his interesting dataset on a Friday afternoon. We did some of the work for the paper on that Friday afternoon, then all went home for a work-free weekend, and came back on Monday to put a full 8 hours of work into the project. Submitted to arXiv just before the daily deadline (18:00 in our time zone). And everybody got to go home on time. I was a little bit worried that maybe lots of other teams would be working through the weekend to publish interesting results from that K2 data release. But it turned out that we were the first people to publish anything from that campaign at all, and the next papers (about different star systems) came out more than 2 weeks after ours. This means that, even in the exoplanet field, one can do one’s work during normal work hours, Monday to Friday, and not be scooped left and right. This makes me much happier about recommending the pursuit of an academic career to my students.
We use cookies to ensure that we give you the best experience on our website. If you continue to use this site we will assume that you are happy with it.Ok
