Today’s blog post is from Dr. Michelle Collins, a Hubble Fellow working at Yale.
After 9 years, 3 billion miles, a Jupiter fly by, and some of the most complex route calculations ever implemented, New Horizons reached its destination a couple of weeks ago on July 14th. This NASA probe went whizzing by our distant, dwarf planet neighbour Pluto at a dizzying speed of 31,000 mph, and has already provided us with a wealth of spectacular images, data and science. It will continue to spew out incredible discoveries about Pluto over the coming 16 months or so, as the flyby data trickles back to us.
To say that this space probe has revolutionized our view of this failed planet is a giant understatement. Pluto has long been an elusive, poorly understood system, hovering on the periphery of our solar system. It was discovered back in 1930 by Clyde Tombaugh, an American working at the Lowell Observatory in Flagstaff Arizona. Due to some miscalculations of the mass of Neptune, it was initially believed that Pluto was a massive planet, at least as big as the Earth, and possibly up to 4 times the size of our home planet. So naturally, it was classified as a planet. However, as the decades wore on, the mass of Pluto was revised downwards, finally lurching to a halt at a mass of only ~0.2% the mass of the Earth in 1978, much lighter than originally thought. With this extreme weight loss, and the discovery of similar size – and even more massive – dwarf planets in the solar system (particularly Eris, discovered in 2005), Pluto’s status as a planet was starting to raise some eyebrows. And so, in 2006, when the International Astronomical Union met to decide what the lower bound on a planet should be defined as, Pluto didn’t make the cut, and was relegated to a dwarf planet.
But, aside from it’s low mass, and controversial status as the only de-throned planet in the Solar System, what else did we know about Pluto, pre-New Horizons? Well, not very much, really. Given it’s huge distance (it’s orbit takes it anywhere between 2.7-4.8 billions miles from the Earth during a single Pluto year), it was hard for us to study Pluto in detail, or take a decent image of it, even with the Hubble Space Telescope. We knew it was an icy world, probably with a rocky core, and maybe underground oceans. It is mostly composed of Nitrogen, with some methane and carbon monoxide. It has an extended, tenuous atmosphere and 5 moons – Charon, Nix, Hydra, Kerberos and Styx. It is locked in a binary orbit with the largest of these, Charon. But the other, smaller moons appeared to us a little more than points of light in Hubble images. If we wanted to learn more about their composition, and that of Pluto itself, we’d need to get A LOT closer to Pluto. And so, New Horizons was constructed and launched on a mammoth journey on 19th January 2006 to our favorite minor planet to get a better look. It was the fastest spacecraft ever launched from Earth, and even managed to image Jupiter and its moons as a bonus science project on its way out to Pluto.
Much of New Horizons journey was spent in hibernation (roughly 7 years), and it was finally awoken on December 6th 2014. From then on, it began imaging Pluto with its onboard cameras, LORRI (a high resolution reflection imager) and Ralph (a multi-filter, lower resolution camera and spectrograph). The combination of these two instruments provided us with incredibly detailed, color images of the surfaces of Pluto and Charon, that got clearer and clearer the closer they got to Pluto. In the weeks before the flyby, we could see that Pluto is a red world, with complex geology. A huge, heart shaped ice plain could be seen on its surface (informally named Tombaugh Reggio after the man who discovered Pluto), and evenly spaced dark spots located on the opposite side of Pluto, which are the size of Missouri, surprised astronomers. Huge craters could also be seen, and regions that seemed surprisingly crater-free too. We also learned that Pluto is a little bigger than we thought, with a radius of 1473 miles, making it larger (though still less massive) than Eris. The sheer variety of surface features, not only on Pluto, but on Charon also, increased the anticipation of the New Horizons team as their target drew nearer, as it was clear that the high resolution flyby would provide them with a treasure trove of answers to the questions already forming.
Tensions were probably pretty high on the day of the flyby itself. After traveling 3 billion miles over 9 years, New Horizons needed to hit a window in space that was only 60×90 miles in size within 100 seconds of its predicted arrival time, otherwise it would miss Pluto. But the orbital calculations were bang on, and New Horizons was able to complete its full range of observations of Pluto and Charon, as well as taking detailed images of Pluto’s 4 other moons. Over the course of a few hours, New Horizons made high resolution maps of segments of both Pluto and Charon, with a maximum resolution of 60 meters per pixel. With that level of detail, you’d be able to count the ponds in central park! In addition to these maps, New Horizons also used several instruments – Alice, REX, PEPSSI and SWAP – to study the atmosphere of Pluto.
So, what else do we know about Pluto now? TONS! For example, the high resolution mapping of Pluto has shown us ice flows on the surface, and evidence for recent geological activity, such as cryovolcanism, which is completely unexpected for such a low mass object that isn’t orbiting a more massive planet. It also has huge mountains ranges, that tower up to 11,000 ft above the surrounding plains. These are most likely composed of water ice.
We also know more about Pluto’s atmosphere. For one thing, the solar wind appears to be stripping it away from Pluto, resulting in a cometary tail-like feature. It also has a hazy quality, where gaseous methane molecules are irradiated by UV light, causing them to condense into complex hydrocarbon molecules known as tholins, which are responsible for the reddish color of Pluto. Its atmosphere also seems to have a lower pressure than previously measured, and could imply that half of it is freezing out and condensing back onto the surface as Pluto segues into its colder season.
We also have high resolution maps of Charon, Pluto’s binary companion. It too, has a geologically young surface, which is totally unexpected for such a small moon. It has a complex set of cliffs, troughs and canyons whose sizes eclipse the Grand Canyon here on Earth. These are thought to be signs of fractured crust on the moon, caused by internal processes. It also has an extended, diffuse dark spot at its pole, informally named ‘Mordor’.
Speaking of moons, we’ve also received the most detailed images of Nix and Hydra from New Horizons. Nix is jelly bean-shaped, approximately 22×26 miles in size, and seems to have a large red spot on one of its faces which may be a crater. Hydra has an irregular shape, that has been compared to the state of Michigan and is about 34 miles in length. It too shows signs of cratering.
And this is only the beginning. There’s much more to come over the next year, and we’re highly anticipating the first ever images of the other 2 Pluto moons, Styx and Kerberos, which should be downloaded in October. There’s more to learn about the surfaces of both Pluto and Charon, with detailed spectroscopy coming in from the Ralph instrument, and more to come on the atmosphere too. So stay tuned to NASA for updates. New Horizons and Pluto have plenty more surprises in store for us, as we learn just how complex and awesome dwarf planets can be.
Today’s guest blogger, Jay Pasachoff, gives us an update (as of July 1, 2015) on his exciting occultation program, first described on May 26, 2015. This is the wild west of astronomy!
Observations of the occultation of June 29, 2015, were very successful both from the ground and from the air. My team has a wonderful light curve from the Mt. John University Observatory in New Zealand; we were close enough to the center of the path that the light curve showed a central peak (a “central flash”), a focusing of starlight as it passed around Pluto, that allowed probing very low in Pluto’s atmosphere. Other teams had light curves from elsewhere in New Zealand and from Tasmania. NASA’s instrumented SOFIA (Stratospheric Observatory for Infrared Astronomy), with its 2.5-m telescope mirror, recorded excellent light curves from high altitude above New Zealand. The views of this occultation will provide excellent comparisons with the ultraviolet and radio occultation results that should be provided by NASA’s New Horizons spacecraft about two weeks later. Further, the long-term run of occultation studies should provide context for the high-quality snapshot view of Pluto’s atmosphere that New Horizons should provide.
Today’s blog is by guest blogger Dr. Jay Pasachoff. Jay is Chair of the International Astronomical Union’s Working Group on Eclipses and is Field Memorial Professor of Astronomy at Williams College. He has viewed 61 solar eclipses, and is an expert on both their use for scientific observations and their use for public education. Jay has has written several astronomy books including the Field Guide to the Stars and Planets and the textbook The Cosmos: Astronomy in the New Millennium. He last provided a blog post about occultations of stars by Pluto in 2011, about a different way of planetary bodies blocking out star light that’s a little closer to home than the exoplanet transits normally discussed in this blog. He’ll be discussing what we can learn from studying dwarf-planet Pluto blocking out (or occulting) the light from distant background stars and relating it to the forthcoming flyby of Pluto by a NASA spacecraft.
As I write, NASA’s New Horizons spacecraft gets closer to Pluto after a 9 year journey. Soon it will give images BTH: Better than Hubble. Already, it is imaging all five known moons of Pluto (http://pluto.jhuapl.edu).
For the last dozen years, my colleagues, students, and I from Williams College have been working with MIT colleagues to observe Neptune’s moon Triton, Pluto, and Charon occult stars–usually stars ranging from 14th to 17th magnitude. The starlight comes into the solar system as parallel light, so the path on Earth from which the occultation is visible is the same width as the occulting object: about 2400 km wide for Pluto and half that for Charon. Our various occultations observed are discussed at a website I set up at http://stellaroccultations.info.
Our group now extends to include Bryce Babcock and me at Williams College; Michael Person, Amanda Bosh, and Carlos Zuluaga at MIT; Amanda Gulbis at the South African Astronomical Observatory; and Stephen Levine at Lowell Observatory, as well as students and others. Carlos posts the MIT group’s latest predictions at http://occult.mit.edu.
I last blogged about our work at the time of a double Pluto/Charon occultation in 2011, which our group observed from several telescopes in Hawaii as well as from the SOFIA aircraft. Our recently published papers that resulted are as follows:
Person, M. J., E. W. Dunham, A. S. Bosh, S. E. Levine, A. A. S. Gulbis, A. M. Zangari, C. A. Zuluaga, J. M. Pasachoff, B. A. Babcock, S. Pandey, D. Amrhein, S. Sallum, D. J. Tholen, P. Collins, T. Bida, B. Taylor, J. Wolf, A. Meyer, E. Pfueller, M. Wiedemann, H.-P. Roeser, R. Lucas, M. Kakkala, J. Ciotti, S. Plunkett, N. Hiraoka, W. Best, E. J. Pilger, M. Miceli, A. Springmann, M. Hicks, B. Thackeray, J. Emery, S. Rapoport, I. Ritchie, M. Pearson, A. Mattingly, J. Brimacombe, D. Gault, R. Jones, R. Nolthenius, J. Broughton, T. Barry, 2013, “The 2011 June 23 Stellar Occultation by Pluto: Airborne and Ground Observations,” Astron. J. 146, 83 (15pp), October, doi:10.1088/0004-6256/146/4/83.
Gulbis, A. A. S., J. P. Emery, M. J. Person, A. S. Bosh, C. A. Zuluaga, J. M. Pasachoff, and B. A. Babcock, 2015, “Observations of the same-day 2011 stellar occultation by Charon and graze by Pluto,” Icarus 246, 226-236. DOI: 10.1016/j.icarus.2014.05.014
Bosh, A. S., M. J. Person, S. E. Levine, C. A. Zuluaga, A. M. Zangari, A. A. S. Gulbis, G. Schaefer, E. W. Dunham, B. A. Babcock, A. B. Davis, J. M. Pasachoff, P. Rojo, E. Servajean, F. Förster, T. Oswalt, D. Batcheldor, D. Bell, P. Bird, D. Fey, T. Fulwider, E. Geisert, D. Hastings, C. Keuhler, T. Mizusawa, P. Solenski, B. Watson, 2015, “The State of Pluto’s Atmosphere in 2013,” Icarus 246, 237-246. http://dx.doi.org/10.1016/j.icarus.2014.03.048
For the ten minutes or so nearest to the occultation for ground-based telescopes, the object and the star appear merged, and we detect the occultation by the light curve. For Charon, with no atmosphere (and our occultation method is very sensitive), the starlight disappears abruptly. If the star is brighter than the occulting object, the occultation is quite noticeable; if the star is fainter, then just a percentage is subtracted from the total. For Pluto (and, earlier, for Triton), its atmosphere bends and distorts the starlight, and the ingress and egress are slanted on the light curve. These ingresses and egresses can last a minute or so with a central occultation of five minutes or so, depending on the relative speed of Pluto with respect to the star.
Astronomical circumstances currently put most of the occultations visible mainly in the southern hemisphere. Last year, in late July 2014, my student Adam Schiff ’15 (Keck Northeast Astronomy Consortium, from Middlebury College), Robert Lucas from Sydney, and I observed from the Mt. John University Observatory of Canterbury University, New Zealand. The observatory is about a 3-hour drive west of Christchurch. We were helped especially by the observatory’s superintendent, Alan Gilmore. Even though the UCAC star catalogue’s values of 15th magnitude for the occulted stars were high by about two magnitudes, we succeeded in observing two occultations by Pluto out of the three we tried. While we were there, we had heard from Wes Fraser of the Herzberg Institute of Astrophysics, Canada (who I knew from when we were both in Mike Brown’s group at Caltech a few years ago) about a prospective occultation by the KBO Quaoar, and also from NZ occultation coordinator David Herald about a prospective occultation by Pluto’s tiny moon Nix; we have flat light curves for both of them–that is, no occultation shadow passed over our site. One needs a dense picket fence of telescopes plus a lot of luck to capture occultations of such small objects. While we were there, we had coordinated observations from Amanda Gulbis with the 4-m telescope on Siding Spring, Australia, and with David Osip on the 6.5-m Clay, Stephen Levine on the 4.1-m SOAR, and Mike Person on the 2.5-m DuPont telescopes in Chile but they, unfortunately, had clouds for the most part.
After our observing run was over in New Zealand, there was another event in Chile, with an especially bright star for us, 12th magnitude. But clouds came in 90 seconds before the predicted ingress. Still, our colleagues noted on the light curve a 2% dip just before the clouds came. Was it from a ring around Pluto? Was it from a hitherto unknown moon of Pluto? It turned out that it was from a previously unknown 15th magnitude star lurking in the Airy disk of the 12th magnitude star, as our colleagues soon confirmed with Keck AO. It was clearly much less exciting to discover a 15th magnitude star than to find a ring around Pluto or to discover a moon. Anyway, we have the light curve of an occultation by that 15th magnitude star, which was the typical brightness of our occultation stars that we were observing anyway. We are about to submit a paper to the Astronomical Journal about our results.
It is important to search in the Pluto system ahead of and behind Pluto itself, since the New Horizons spacecraft’s radio signals are so weak that it will take 18 months or so after the July 14, 2015, flyby to send back all the data (from about 40 au; at 8 light minutes per au, it takes over 5 hours to get signals back at all). So if the spacecraft is killed at flyby by running into a ring particle or other dust, then most of the data–even from closest approach–would be lost. Our earlier occultation observations provided some limits on the dust content, and were among many pieces of evidence considered by the New Horizons team at Southwest Research Institute, headed by Alan Stern, in targeting their spacecraft.
We actually don’t know exactly how big Pluto is, because its lower atmosphere is opaque to starlight during occultations. It could be from haze in the lower atmosphere or thermal inversion. Eris, on the other hand, is so far out that its atmosphere has frozen and snowed onto the surface. We therefore now know from occultation studies by the Bruno Sicardy group from Paris just how big Eris is, and it turns out to be near the lower end of the possible range of Pluto’s size. Would the IAU have reclassified Pluto as a dwarf planet in 2006 if Pluto hadn’t been thought to be smaller than Eris? (It is certainly less massive, since each has at least one moon that has provided an accurate mass value.) Would NASA have launched a spacecraft to Pluto if it hadn’t been thought to be the 9th, and the only unvisited, planet?
We have a prediction this year for the occultation of a 12th magnitude star from the region of New Zealand, and perhaps the lower half of Australia. (http://occult.mit.edu/research/occultations/Pluto/P20150629) If you can observe from the centerline, you might get a central flash from focusing of the starlight all around Pluto–as we once got (with much luck) from Hubble. With this desirable possibility in mind, NASA’s SOFIA (Stratospheric Observatory for Infrared Astronomy) will fly out of Christchurch, with Mike Person from our group on board. Amanda Bosh will be in Flagstaff, coordinating last-minute updates to the astrometry. Bryce Babcock and I will be at Mt. John, with our Williams College undergraduates Rebecca Durst ’17 and Christina Seeger ’16; Alan Gilmore will continue to assist us, even though he has retired. This time, we have not only the 1-m telescope but also an adjacent 0.6-m telescope, for which Stephen Levine will bring down an infrared camera from our Williams College alumnus Henry Roe who is now at the Lowell Observatory. We even have arranged with a Japanese group who use a second 0.6-m telescope to get three-color photometry from it, unless they have an urgent need for it as part of their gravitational-lensing program. Amanda Gulbis will be observing from a different location in New Zealand, to give us a different chord. The Southwest Research Institute (SwRI), especially Leslie Young and Eliot Young, have also arranged observations from telescopes around Australia and New Zealand, just as we are coordinating with other telescopes besides those at Mt. John. The Bruno Sicardy group from Paris also has its own prediction.
It could be particularly important and interesting to be observing so close to the July 14 flyby by New Horizons, since then we can compare results taken at a comparable state of Pluto’s atmosphere. The atmosphere of Pluto, far from snowing out by now even though it passed perihelion in 1989, had warmed slightly and had increased pressure by the time of our 2002 observations, and has since leveled off. There will certainly be enough atmosphere for New Horizons to observe, which had not been clear a dozen years ago. It must start cooling at some point, as Pluto recedes from the Sun. We hope to calibrate our atmospheric models with the new size of Pluto we will get from New Horizons, and to follow Pluto’s atmosphere as it continues to evolve.
Our occultation work at Williams College has been sponsored by grants from NASA’s Planetary Sciences Division, most recently NNX12AJ29G.
13 May 2015
Thank you to everyone who has participated up to this point! The votes have been counted and Planet Hunters has submitted the following naming suggestion to the IAU ExoWorld naming contest:
- PSR 1257 12: Photo – Photo is the Greek word for light. Since it is a pulsar that releases two beams of light, Photo would be suitable as a name that emphasizes the beams of light the pulsar emits.
- PSR 1257 12b: Lofío – Since b is the least massive exoplanet ever discovered, the Greek word for a plume fits. Naming the least dense exoplanet after a feather honestly seems suitable.
- PSR 1257 12c: Xekiní̱ste – Since this is one of the first exoplanets discovered, the Greek word for start fits. This name signifies the start of a new era in finding planets outside of our solar system.
- PSR 1257 12d: Amydrós – Since it is the outermost planet in the system, it has the longest orbit; it blocks the light beams the most. So for that reason, the Greek word for dim fits, as it dims out the pulsar beams the most.
A hardy congratulations to Trent Crespo is in order. It was his name that was decided on by this community to put forward!
Our work is not done though – shortly in June 2015 a sign-up window will open for individuals to register to vote for the IAU naming selection. Watch http://www.nameexoworlds.org/#signup for this window to open!
The group has done a fantastic job voting so far! For the final days of this vote, I have narrowed down the list of options to the top 4! This four options had greater than 10% of the vote. The voting page has been updated once again and we are asking you to select one naming suggestion for us to move forward to the IAU. If you voted previously, you can vote again. Voting for this round will be ended on May 15, 2015, so please vote promptly!
On April 16, 2015, the gavel was slapped on round 2. The naming suggestions were reviewed by Planet Hunter moderators for conformance to the IAU criteria and in all the community had generated 33 naming suggestions that appear to conform. Now it is time for round 3! The voting page has been updated once again and we are asking you to select one naming suggestion for us to move forward to the IAU. Voting for this round will be ended on May 15, 2015, so please vote promptly!
In the blog post earlier today, I reported that phase 1 was complete – the IAU (International Astronomical Union) has selected the stars to be named. Phase 2 involves groups providing naming suggestions for the star and all attached planets. The “Vote” button has been updated with a new form to begin taking these suggestions from Planet Hunters! Please provide your naming suggestion by April 16, 2015.
After April 16, 2015, the Planet Hunter’s moderators will review the suggestions for conformance to the stated guidelines for naming suggestions and a poll will be set up for us to select our one naming suggestion that will be put up. So start your suggesting!
Proposed names should be:
- 16 characters or less in length.
- Preferably one word.
- Pronounceable (in some language)
- Not too similar to an existing name of an astronomical object. Names already assigned to astronomical objects can be checked using the links http://cds.u-strasbg.fr/cgi-bin/sesame (for galactic and extragalactic names), and the MPC database http://www.minorplanetcenter.net/db_search (for names)
In addition it is not allowed to propose:
- Names of pet animals.
- Names of a purely or principally commercial nature.
- Names of individuals, places or events principally known for political, military or religious activities.
- Names of living individuals.
- Only names that are not protected by trademarks or other forms of intellectual property claims may be proposed.
As you are likely aware, Planet Hunters is taking part in an IAU (International Astronomical Union) project to name several ExoWorlds. A few months back we provided the IAU a list of ExoWorlds which we thought should be named. The IAU took this list, plus all of the lists provided by other groups and determined which ExoWorlds will be named. In total, 15 stars and 32 planets will be named. The list:
|Host Star (catalogue)||# Planet (designation)||Planet Mass (Jupiter mass)||Planet Mass (Earth mass)||Orbital Period (day)||Semi Major Axis (au)||Discovery (year)||Constellation (English)||Visibility||V magnitude|
|1 exoplanet (5 systems)|
|Ain (epsilon Tauri)||epsilon Tauri b||7.6||2415.5||594.9||1.93||2007||the Bull||Visible to the naked eye||3.5|
|Edasich (iota Draconis)||iota Draconis b||8.82||2803.3||510.7||1.275||2002||the Dragon||Visible to the naked eye||3.3|
|Errai (gamma Cephei)||gamma Cephei b||1.85||588||903.3||2.05||2003||the King||Visible to the naked eye||3.2|
|Fomalhaut (alpha Piscis Austrini)||Fomalhaut b||3||953.5||320000||115||2008||the Southern Fish||Visible to the naked eye||1.2|
|Pollux (beta Geminorum)||beta Geminorum b||2.9||921.7||589.64||1.69||2006||the Twins||Visible to the naked eye||1.2|
|1 star + 1 exoplanet (10 systems)|
|14 Andromedae||14 Andromedae b||5.33||1694||185.84||0.83||2008||the Chained Maiden||Visible to the naked eye||5.2|
|18 Delphinis||18 Delphinis b||10.3||3273.6||993.3||2.6||2008||the Dolphin||Faint to the naked eye||5.5|
|42 Draconis||42 Draconis b||3.88||1233.2||479.1||1.19||2008||the Dragon||Visible to the naked eye||4.8|
|51 Pegasi||51 Pegasi b||0.47||148.7||4.23||0.052||1995||the Winged Horse||Visible to the naked eye||5.5|
|epsilon Eridani||epsilon Eridani b||1.55||492.6||2502||3.39||2000||the River||Visible to the naked eye||3.7|
|HD 104985||HD 104985 b||6.3||2002.3||198.2||0.78||2003||the Giraffe||Faint to the naked eye||5.8|
|HD 149026||HD 149026 b||0.36||113.1||2.88||0.04288||2005||the Hercules||Visible through binocular||8.2|
|HD 81688||HD 81688 b||2.7||858.1||184.02||0.81||2008||the Great Bear||Visible to the naked eye||5.4|
|ksi Aquilae||ksi Aquilae b||2.8||889.9||136.75||0.68||2008||the Eagle||Visible to the naked eye||4.7|
|tau Bootis||tau Bootis b||5.9||1875.2||3.31||0.046||1996||the Herdsman||Visible to the naked eye||4.5|
|1 star + 2 exoplanets (1 system)|
47 Ursae Majoris
|47 Ursae Majoris b||2.53||804.1||1078||2.1||1996||the Great Bear||Visible to the naked eye||5.1|
|47 Ursae Majoris c||0.54||171.6||2391||3.6||2001||the Great Bear||Visible to the naked eye||5.1|
|1 star + 3 exoplanets (2 systems)|
PSR 1257 12
|PSR 1257 12 b||7.00E-05||0.022||25.26||0.19||1992||the Maiden|
|PSR 1257 12 c||0.01||4.1||66.54||0.36||1992||the Maiden|
|PSR 1257 12 d||0.01||3.8||98.21||0.46||1992||the Maiden|
|upsilon Andromedae b||0.62||197.1||4.62||0.059||1996||the Chained Maiden||Visible to the naked eye||4.1|
|upsilon Andromedae c||1.8||572.1||237.7||0.861||1999||the Chained Maiden||Visible to the naked eye||4.1|
|upsilon Andromedae d||10.19||3238.7||1302.61||2.55||1999||the Chained Maiden||Visible to the naked eye||4.1|
|1 star + 4 exoplanets (1 system)|
|mu Arae b||1.68||532.7||643.25||1.5||2000||the Altar||Visible to the naked eye||5.2|
|mu Arae c||0.03||10.6||9.64||0.09094||2004||the Altar||Visible to the naked eye||5.2|
|mu Arae d||0.52||165.9||310.55||0.921||2004||the Altar||Visible to the naked eye||5.2|
|mu Arae e||1.81||576.5||4205.8||5.235||2006||the Altar||Visible to the naked eye||5.2|
|1 star + 5 exoplanets (1 system)|
|55 Cancri b||0.8||254.3||14.65||0.1134||1996||the Crab||Faint to the naked eye||6|
|55 Cancri c||0.17||53.7||44.34||0.2403||2002||the Crab||Faint to the naked eye||6|
|55 Cancri d||3.84||1218.9||5218||5.76||2002||the Crab||Faint to the naked eye||6|
|55 Cancri e||0.03||8.3||0.74||0.0156||2004||the Crab||Faint to the naked eye||6|
|55 Cancri f||0.14||45.8||260.7||0.781||2007||the Crab||Faint to the naked eye||6|
At this point, Planet Hunters can submit one naming suggestion. A suggestion consists of the name for one star, all attached planets and the basis for this recommendation. We are working to set up a Google form to select submissions and then we will have a round of voting to select the candidate to be submitted. This will all take place prior to May 31, 2015.
A new MAST High Level Science Product from K2 has been delivered that includes extracted lightcurves. Courtesy of Vanderburg & Johnson (2014), long-cadence targets from Campaigns 0 and 1 now have detrended, extracted lightcurves available at MAST, including 20 different photometric apertures. There’s a MAST Classic Search Interface so you can get lightcurves based on target IDs, coordinates, EPIC catalog fluxes, etc. You can also use our interactive plotter to explore the lightcurves using any of the photometric apertures before downloading the FITS files. Check out all the details here: http://archive.stsci.edu/prepds/k2sff/