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2016A Proposals

Click the title of each proposal to read the abstract

Science Collaboration Key Projects (includes time from all Partners)

Title PI name PI Institution Hours (2m) Hours (1m) Hours (0m4)
Echo Mapping of AGN Accretion Flows Horne, K. St. Andrews U. 245 685 0
Our goals are to measure black hole masses and quasar distances out to redshift ~2 by exploiting light travel time delays to resolve micro-arcsecond structure of accretion flows onto supermassive black holes in active galactic nuclei (AGN). LCOGT is the enabling technology for mass production AGN echo mapping, with FLOYDS for spectroscopy and the 1m scopes for imaging, providing long high-cadence lightcurves. Time delays from the lightcurves give us the radii of emission line and continuum regions around the accreting black hole. The emission-line widths and time delays (weeks-months) give us the black hole mass (Mbh). We will measure Mbh at high redshift by monitoring Hbeta+MgII for 10 AGN at z~0.35, MgII+CIV for 10 at z~1.6, and CIV for 2 lensed quasars at z=2-2.3. We then calibrate the Hbeta+MgII+CIV size-luminosity relations to find Mbh for thousands more AGN. To measure quasar distances, we will use the LCOGT 1m scopes for ugriz lightcurves and measure continuum delays (days) increasing from blue to red, thus probing the accretion disk T(R) profiles, measuring accretion rates (M dM/dt), and distances (D). With D for ~70 quasars out to z~2 we can independently probe the cosmic expansion history with different systematics and at higher redshifts than Type Ia supernovae. If NASA approves the Kepler 2 ecliptic plane survey, we will exploit the unique opportunity to target AGN in the K2 fields.
The Next-Generation Sample of Supernovae Howell, A. LCOGT 280 845 0
In the study of supernovae, we are leaving the serendipity era, when we had to learn from what nature provided by chance, and entering the database-driven era, when we can ask questions by comparing statistically significant groups of supernovae. This project will obtain light curves and spectra of 100 Type Ia and 100 core-collapse supernovae per year over three years. We will start light curves and spectroscopy within hours of discovery, and focus on those SNe caught soon after explosion. The goals are fivefold: (1) observe supernovae soon after explosion to search for signs of their progenitors, (2) obtain a large homogeneous sample of supernovae for next generation cosmological studies, (3) obtain a large sample of supernovae for statistical studies comparing groups that are split into different populations, (4) obtain some of the first large samples of the recently discovered classes of rare and exotic explosions, (5) obtain the optical light curves and spectroscopy in support of studies at other wavelengths and using other facilities including UV observations, IR imaging and spectroscopy, host galaxy studies, high resolution spectroscopy, and late-time spectroscopy with large telescopes.
Exploring Cool Planets Beyond the Snowline Street, R. LCOGT 100 2552 0

This proposal aims to explore the one regime in exoplanetary science which remains hardly touched: the population of planets of all masses predicted to form in the cold outer reaches of planetary systems between 0.5-10AU, but which are difficult or impossible to find by most planet hunting techniques. Microlensing is uniquely sensitive to this parameter space and has proven capable of detecting even Earth-mass planets from ground-based observations alone. But to fully characterize these unpredictable and non-repeating events demands high precision photometry with 24/7 monitoring over several weeks, as well as highly responsive scheduling and great flexibility to handle the rapidly evolving targetlist. LCOGT's robotic, queue-scheduled network is ideal. Over the last few years, our team have developed a unique system designed to take maximum advantage of LCOGT's resources in order to detect and characterize cool planets discovered from the subtle photometric anomalies they cause in microlensing lightcurves. Over the course of this Key Project we will double the number of known cool and low mass exoplanets, a population that is a critical test of planetary formation models.

Outer Solar System Studies Bianco, F. NYU 57 78 0

This proposal aims to investigate the Outer Solar System (OSS) with a synergic photometry, spectroscopy and high speed photometry program, which will organize various programs already running at LCOGT with new scientific approaches at a critical time for the study of the OSS, with the New Horizons spacecraft approaching Pluto, Pluto transiting crowded fields, increasing dramatically the rate of occultations, and the coming online of the OSS Origins Survey (OSSOS). The program has two main lines of scientific inquiry: 1) Observe occultations of Pluto over three years in several passbands simultaneously, using LCOGT’s unique capability of having 2-3 telescopes equipped with fast cameras at a single site, and potentially multiple identical sites within a track. We aim to probe the evolution of Pluto’s atmosphere, and support the New Horizons space mission for the years before, during and after the July 2015 encounter. Obtain three-color (B,V, r’) light curves (and associated calibration star-field data) of Pluto, and time-resolved low resolution spectroscopy using FLOYDS to produce constraints on the evolution of Pluto’s atmosphere & surface. 2) Observe occultations of large TNOs, including new discoveries from OSSOS, to gain crucial information about the distribution of sizes, albedos, shapes, densities and thermal inertia & temperatures. Constraints on the surface and atmosphere of Pluto, and on the statistics of TNOs are very powerful tools to constraint SS evolution.

LCOGT, Inc.

Title PI name PI Institution Hours (2m) Hours (1m) Hours (0m4)
Searching for Optical Counterparts to Gravitational Waves Arcavi, I. LCOGT 50    
We propose to use the LCOGT 2m telescopes to search for optical counterparts of gravitational waves (GWs) detected during the upcoming advanced LIGO+Virgo observing run 2 (O2). Finding a counterpart will identify the source of the GWs and will help maximize the science produced from the GW detection. The number of galaxies containing 50% of the mass inside a LIGO+Virgo error region during O2 is expected to be 20-30. We will be able to visit all of these galaxies with an LCOGT 2-meter in a single night, and to re-visit them for several consecutive nights with a modest time allocation. With this strategy, a large field of view is not required, but rather rapid-trigger robotic telescopes have the advantage. LCOGT, as the only operator of robotic 2m-class telescopes capable of rapid response in both hemispheres and as a member of the LIGO followup collaboration, is ideal for carrying out this search. While the number of GW triggers during the overlap between O2 and LCOGT semester 2016A is expected to be small (~1), there is potential for a highly significant discovery. In future runs, LIGO and Virgo's detection range will increase but the size of the error-region will decrease, leaving the number of galaxies in the search region roughly the same. The current semester thus provides an opportunity to develop the expertise and techniques that will allow LCOGT to be an important contributor to GW-counterpart searches when LIGO and Virgo reach their full sensitivity.
Classification and Followup of Tidal Disruption Events Arcavi, I. LCOGT 78 56  
Tidal Disruption Events (TDEs), the disruptions of stars by supermassive black holes (SMBHs), are now being discovered in real time by optical transient surveys. Recently we found that TDEs exhibit a continuum of spectral properties and that they strongly prefer post-starburst host galaxies. Our classification scheme has aided in the identification of new events, yet the physical mechanisms responsible for the observed emission are not yet understood. LCOGT observations are crucial to nailing down the multi-wavelength properties of TDE emission, in conjunction with radio, UV and X-ray data. New events will also help us investigate the surprising host-galaxy preference shown by TDEs. In 2015B we began a dedicated TDE survey with LCOGT to find more events (the survey, called "SEATiDE", runs through 2016A). Here we propose to continue our successful LCOGT TDE classification and followup program which has so far collected valuable data on several confirmed TDEs. We aim to classify TDE candidates and to collect well-sampled photometry and spectroscopy of three new confirmed TDEs to be discovered during 2016A by SEATiDE and other surveys (e.g. public surveys like ASAS-SN and OGLE, and surveys we have access to as members of the LCOGT Supernova Key Project like iPTF and LSQ). Continuing to discover and follow new TDEs will help map their diversity, a first step towards constraining their physics and enabling their use as a new tool to study otherwise quiescent SMBHs.
Rotational properties of spacecraft target asteroid (162173) 1999 JU3 Greenstreet, S. LCOGT 48    
We propose to conduct a photometric study of the Japan Aerospace Exploration Agency's (JAXA) Hayabusa 2 mission target asteroid (162173) 1999 JU3 using the LCOGT 2.0-m network. The Hayabusa 2 spacecraft was launched successfully in December 2014. It is expected to arrive at 1999 JU3 in mid-2018 and subsequently return to the Earth with a sample from the asteroid in 2020. Knowing the asteroid's physical characteristics, such as its rotational period, shape, and pole orientation, is essential not only for mission sequencing but for ensuring the safety and fuel efficiency of landing on the asteroid, collecting the sample, and returning to Earth. Currently, the spin axis and shape model of 1999 JU3 are not well constrained due to large uncertainties in the photometric data and the small lightcurve amplitude, which likely indicates it has a spheroidal shape with an axial ratio a/b = 1.12. Therefore, high quality (S/N > 100), well-sampled photometric data are required to confirm the asteroid's rotational period and better constrain the pole solution. The observation window in mid-2016 is the last chance to observe 1999 JU3 before the arrival of the Hayabusa 2 spacecraft in mid-2018.
Continuous Observations of Disintegrating, Transiting Planetesimals around a White Dwarf Eastman, J. Harvard CfA   90  
We propose to obtain continuous photometry of the disintegrating planetesimals orbiting the white dwarf WD 1145+017 using the unique longitudinal coverage of the LCOGT network of 1-meter class telescopes. It is believed that the transit events that are observed in the WD 1145+017 system are due to small chunks being tidally ripped off a "main" asteroid; these chunks then disintegrate in a matter of weeks. The unique continuous coverage offered by the LCOGT network will allow us to track the lifetime of these objects by investigating the orbit-to-orbit evolution of the transit profiles and depths, which will help to identify the disintegration mechanism. The transit events we observe in the WD 1145+017 evolve from orbit-to-orbit, night-to-night and season-to-season and therefore our request for multiple nights of coverage will help constrain the physical mechanism leading to these night-to-night and orbit-to-orbit differences. Finally, by coordinating with previously allotted telescope coverage of this system, we will be able to perform multiwavelength observations and therefore determine the particle sizes in the cometary tails streaming behind the planetesimals in this system. Constraints on the particle sizes will better to determine the disintegration mechanism (collisions, tidal disruption, a thermal wind, etc.) that has led to both the cometary tails and the arrival of these planetesimals in such short period orbits.
Image Subtraction Templates for Supernovae McCully, C. LCOGT 27 94  
To unlock the full scientific potential of the LCOGT supernova (SN) data set, accurate photometry is a necessity. For most of the SN sample, this requires removing host galaxy contamination by subtracting supernova-free template images from the original observations. Here, we propose to obtain reference images for SNe discovered in the second year of the SN Key project. With the data from this proposal, we will be able to build quality SN light curves and measure SN host galaxy properties. This will enable a variety of SN science, including SN Ia cosmology, SN companion shocking, resolving the worrying difference in corrected luminosities seen in SNe Ia in different galaxy types, and probing the physics behind the explosions of massive stars.
Understanding Free-Floating Planets Street, R. LCOGT   200  
The existence of free-floating planets is predicted by a number of planetary formation and migration models, but these extremely faint objects are hard to find or study in detail. Microlensing offers an efficient way to survey for these objects, but to measure their physical properties we first have to measure their parallax. This is challenging, since the timescale for these transient events (<2 days) does not allow Earth to move far enough in its orbit. However, in 2016, K2/Campaign 9 will continuously observe a portion of the Galactic Bulge from a distance of ~0.5AU from Earth. The LCOGT Microlensing Key Project has dedicated its existing allocation to conducting a simultaneous survey of this region as part of a global follow-up program that includes 4 Keck ToO triggers, as well as dense monitoring of targets outside this region. This is a unique opportunity to determine masses for free-floating planet candidates. However, survey event alerts for these targets have a high false alarm rate, so urgent, two color imaging of candidates is needed in real-time in order to make the most effective use of the Keck time. LCOGT is the ideal facility to provide this urgent-alert response, complementing the aims of the ongoing Key Project.
Monitoring Stellar Activity for Exoplanet Hosts: Essential Support for a Gemini Survey Program Huitson, C. U. Colorado   56  
We propose nightly photometric monitoring of 4 exoplanet host stars with the 1-m network; a continuation of program LCO2015B-003. The proposed program is essential to the success of an accepted Gemini survey, which is the first aimed at characterization of exoplanet clouds. Since understanding clouds is essential to measuring exoplanet compositions, this an important step forward in the field of exoplanet science. The Gemini survey will measure scattering signatures in blue optical transmission spectra during multiple observations to determine cloud species. However, while the blue optical is the only spectral region where clouds can be directly detected, it is also the spectral region where stellar activity produces strong signals in transmission. The proposed LCOGT program is essential in order to dis-entangle contaminating stellar signals from true planetary signals. The stellar contribution varies significantly depending on the number of starspots visible, and only independent measurements of the stellar spot level will enable distinction between the two signals. Long-term, frequent, photometric monitoring throughout the Gemini survey is the only way to measure the stellar spot level at the time of each transit event, by allowing us to model the stellar periodicity, spot evolution and estimate the non-spotted stellar brightness. This is the only way to correct the transmission spectra for stellar effects and accurately characterize the planetary cloud species.
Long Baseline Transit Timing of Low-Mass Planets Beyond the Range of RV Street, R. LCOGT 18 37  
We propose targeted ground-based follow-up of Kepler’s long period transiting planets with detected transit timing variations (TTV) to constrain the masses of low-mass planets, all of which are too low in mass for detectable RV signals, and all of would benefit from transit data beyond the four-year Kepler baseline. Future transit data will significantly improve constraints on the masses and densities of these planets compared with what is possible from the Kepler dataset. Two of our targets are notable for having extreme low densities for planets below 25MEarth. These planets are high profile targets for planet formation models and JWST spectroscopy. They have longer orbital periods than any other transiting planets that have been observed from the ground. Hence, with its flexibility in geographic longitude, LCOGT is uniquely capable of taking these observations.
Completing Our Census of Accretion in Young Binaries Ciardi, D. NExSci/Caltech   69  
Most stars form in binaries, and the evolution of protostellar disks in pre-main-sequence (PMS) binary stars is a current frontier of star formation research. PMS binary stars can have up to three accretion disks: two circumstellar disks and a circumbinary disk separated by a dynamically cleared gap. Theory suggests that mass may flow in an accretion stream from a circumbinary disk across the gap to circumstellar disks or stellar surfaces. The accretion rates should be dynamically modulated on the orbital period. Continuous, multi-orbit, multi-color photometric observations with dense phase coverage are required to detect and characterize these modulated accretion streams, if they are generally present. The 1-m LCOGT network is designed for this observational challenge, and we propose to study two choice PMS binaries (P < 90 days) with active accretion and protostellar disks. Each binary will be observed 20 times per orbit in U,B,V,R,I,Y, and in Ha and Hb filters. This unprecedented wealth of data will directly test the predicted phase modulations of accretion streams, determine accretion luminosities, and reveal the presence of accretion hot spots, all as a function of orbital parameters. These observations will guide an extension of the accretion paradigm from single young stars to multiple systems and inform the physics of planetary growth around single and binary stars.
Fundamental Properties of Low Mass Stars in Eclipsing Binaries Hebb, L. Hobart & William Smith Colleges   159  
We request a total of 159 hours with the LCOGT 1m network to obtain SDSS g' and i' light curves of 24 low-mass M dwarfs in eclipsing binaries with F/G/K primaries. This is part of a larger effort to constrain the mass-radius-temperature relation as a function of activity and metallicity at the bottom of the main sequence with unprecedented large number statistics. With these observations, we will determine the precise radii of the M dwarfs in our sample. The comprehensive modeling of the binaries, including existing radial velocity curves of all our targets, will allow us to fully determine their fundamental properties, including masses, radii and metallicities. We will observe the secondary eclipses for a subset of the targets where the flux ratio is amenable in order to obtain secondary star temperatures for these particular objects.
Rotation Periods for Rapidly Rotating L Dwarfs and a Test of Spin-Orbit Alignment Burgasser, A. UCSD 119    
The surfaces of L-type dwarfs have been shown to exhibit asymmetries, either from magnetic spots or cloud features, which manifest as rotationally-synched periodic and aperiodic variability. Various studies have examined how temperature, surface gravity and rotation rate influence these dynamics. However, a confounding factor is the orientation of the spin axis, which is rarely known due to the lack of combined high-resolution spectroscopy and time-series photometry. Over the past 6 years we have conducted a high-resolution spectroscopic survey of L-type dwarfs with Keck/NIRSPEC which have provided several dozen v sin i measurements. We propose monitoring the most rapidly rotating of these to search for periodic variability and measure spin axis orientation. One of our targets, SDSS 0805+4812, is also a tight binaries with a well constrained orbital inclination, which we will compare to spin orientation measurements to make the first test of spin-orbit alignment in the substellar regime.
Follow-Up Observations of KOI-89 van Eyken, J. IPAC   9 10
KOI-89 is a two-planet system transiting an A-type star that was first discovered and charac- terized through Kepler photometry from 2009-2013. Ahlers et al. (2015) measured the two planets’ orbital planes to be nearly perpendicular to the star’s equatorial plane, making this system a valuable tool for testing spin-orbit misalignment hypotheses. However, the discov- ery data suggests a dynamically complex system that can only be fully understood through additional observation. Specifically, the two planets are undergoing large-amplitude, asinu- soidal transit timing variations, indicating that there are additional planets in the system. We therefore propose to extend KOI-89.01’s baseline of measured transit events, which will play a key role in determining the total number of planets in this system and in constraining their masses, shedding new light on KOI-89’s dynamic behavior and formation history.
Multisite observations of the pulsating central star of the Planetary Nebula Abell 43 Jones, D. IAC 20 30  
Up to 98% of all single stars will eventually become white dwarfs, stars that link the history and future evolution of the Galaxy, and whose previous evolution is engraved in their interiors. These interiors can be studied using asteroseismology, utilizing stellar pulsations as seismic waves. For the most "unevolved" group of pulsating (pre-)white dwarf stars asteroseismology became possible already 25 years ago, but only a small number of these stars can be regarded as satisfactorily studied. This may be partly due to many representatives still being surrounded by bright Planetary Nebulae making the required observations - high-precision time-resolved photometry - challenging. We have therefore embarked on a systematic seismic study of pulsating Planetary Nebula Central Stars using image subtraction techniques which negate the nebula contamination which plagued previous works. The present proposal is part of a worldwide campaign on the central star of Abell 43 - a central star that has just entered the PG1159 instability strip, and which offers the opportunity to study this phase in more detail than ever before. The proposed LCOGT observations will form an integral part of this multisite study.
Photometric monitoring of bright stars hosting small planets IV Dragomir, D. LCOGT   178  
Ongoing transit surveys such as Kepler have resulted in the discovery of nearly three dozen small exoplanets with measured masses and radii. Yet the majority of these planets are challenging targets for atmospheric characterization studies. Our team has an approved large HST program aiming to probe the atmospheres of the six small planets most amenable to such a study. We will obtain transmission spectra at visible and infrared wavelengths with unprecedented precision, increasing by a factor of a few the number of well-characterized small exoplanets. We propose to use the LCOGT network to photometrically monitor the host stars of these systems for the duration of the HST program (fall 2014 to spring 2016). Four-color LCOGT photometry over this duration will help us understand how the variability of the host stars changes between transits. These multi-band data will be used to constrain the temperature of the star spots and the stellar variability at multiple wavelengths. With these measurements we will correct the STIS and WFC3 transmission spectra, ensuring an accurate interpretation of these spectra which will allow us to robustly determine the atmospheric properties and composition of these small planets.
Characterizing Planets in the Solar Neighborhood Siverd, R. LCOGT 30 150 100
The most scientifically productive exoplanet discoveries are transiting planets orbiting bright host stars. These are the only ones for which accurate physical parameters (radii, masses, densities, temperatures, compositions) can be determined. However, only ~2% of the ~1300 transiting planets have host stars that are sufficiently bright for such detailed studies. Wide-field photometric transit surveys are best able to provide a statistically significant sample of planets around nearby, bright stars but their candidates require follow-up observations to vet candidates and properly characterize promising systems. The KELT project is such a survey that targets primarily FGK stars with V ~7.5-11 mag. KELT has already published several planetary discoveries from its Northern and Southern telescopes using data from LCOGT, and several more discoveries are in preparation. The Southern LCOGT nodes have been especially critical in the discovery of these planets as the KELT network has much fewer follow-up partners in the South than in the North. We propose to continue our successful program to obtain high precision photometry of KELT candidates and therefore support the discovery of transiting planets around bright stars that are ripe for detailed characterization, especially with the upcoming James Webb Space Telescope.
Phase Curves and Spectral Types: The Extreme Opposition Surge of Asteroids Bauer, J. IPAC   175  
The reflectivity of solar system surfaces spikes sharply when the Sun is directly behind the observer. Spacecraft measured this ‘opposition surge’ for icy outer planet satellites and discovered that the reflectivity of part of Europa’s surface increases by as much as a factor of 8 as the observer moves from 5 deg to the exact backscattering direction! One mechanism explains this spike as coherent light scattering that occurs only at this unique retro-reflection geometry. Due to the tight linear alignment of the target, observer and Sun required to measure the peak brightness of the spike, accurate and complete measurements of the amplitude and decay of the spike exist for only a few targets. We request 175 hours of 1-m time to use the unique capabilities of LCOGT to systematically measure this extreme opposition surge for 31 asteroids with a variety of compositions. Each asteroid will be observed in r’ and g’ during the ~8 hour interval when it passes within ~0.1 deg of the point opposite the Sun on the sky. Supporting observations measure asteroid rotation and phase angle brightness changes to enable accurate characterization of the spike. This data set will significantly increase the number and variety of the surfaces, and measurement accuracy compared to existing asteroid data. We will determine how the spike characteristics vary with surface composition, albedo and wavelength providing new constraints on physical models of this ubiquitous yet poorly understood phenomenon.
Probing asteroid families with precise photometry Lister, T. LCOGT   257  
Asteroid families are products of catastrophic collisions, and their properties are a very important input for modelling the physics which governs these phenomena and understanding the evolution of the early Solar System and potentially other exoplanetary systems. The use of new techniques for computing the proper elements of large number of asteroids and hierarchical clustering methods to identify new, and refine existing, families enables us to extract a great deal of information, in particular the ages of the formation of these collisional families. A drawback of these large samples is that the absolute magnitude, which is used to derive the diameter and age, is drawn from a very inhomogeneous source (the Minor Planet Center’s database) with typical scatter of greater than 0.25 mag. We wish to continue to use the LCOGT Network to obtain precise calibrated photometry of a subset of the Vesta asteroid family to provide better constraints on the age of this important dynamical family. The refined absolute magnitude will allow more accurate diameters and ages for the two major collisions that formed this family. This will enable a cross-comparison on these ages with those derived from the cratering ages from images returned by the Dawn spacecraft. This proposal will build on the pilot program in 2015B to cover a broader range of phase angles and provide a more sensitive search for rotational variations which could bias the derived absolute magnitudes.
BRing, BRing: searching for exorings around the brightest directly imaged exoplanet beta Pictoris b Kenworthy, M. Leiden Obs.   30 50
We propose a monitoring campaign of the bright Southern hemisphere star beta Pictoris in 2016 and 2017 to look for the transit of the gas giant planet beta Pictoris b and any circumplanetary rings and material within the gravitational influence (the Hill sphere) of the planet. The star system is young (23 Myr) and has a famous edge­on debris disk, complete with a ~10 Jupiter mass gas giant planet in a 20­30 year orbital period at about 5AU orbit from the star, also with an orbit that is edge­on to our line of sight. Previous photometric observations in 1981 show 6% photometric fluctuations over several days, at an epoch consistent with a previous inferior conjunction of the planet. Recent direct imaging observations show the angular separation decreasing between the star and planet, and in the next six to twelve months, the Hill sphere of the planet will start to move between us and the central star. The longitudinal coverage of LCOGT will enable monitoring for the primary transit, and any giant rings around the central planet. Nightly observations of beta Pictoris will enable the triggering of intensive observations if and when we see circumplanetary material begin to transit.
Post-Jupiter Encounter Light Curves of C/2015 ER61 (PANSTARRS) Holler, B. U. Colorado 6 12  
The recently re-classified C/2015 ER61 (PANSTARRS) will pass within 1 AU of Jupiter in late March 2016. This minor body was discovered in March 2015 and has an orbital period of 50,000 years. Observations with the LCOGT are currently underway to observe this object in order to determine a pre-encounter rotation period. We propose to continue these observations in the 2016A semester to compare rotation periods and determine if a change occurred as a result of the gravitational interaction with Jupiter. The absolute magnitude, diameter, and mass will also be determined or estimated. Astrometry of this object will enable a re-calculation of its orbital parameters post-encounter. It is possible shape and axial orientation can be extracted from the light curve. Our strategy is to observe 2015 ER61 over three 48-hour periods, with one each in April, May, and June 2016. Both the 1m (SBIG) and 2m (Spectral) class telescopes will be used to obtain images of 2015 ER61 in the SDSS r band. 2015 ER61 will be at an apparent V magnitude of 19 during this time period, and brighter in the r band.
LCOGT NEO Follow-up Network Lister, T. LCOGT 20 225 200
Near Earth Objects (NEOs) are our closest neighbors and research into them is important not only for understanding the Solar Systems’ origin and evolution, but also to understand and protect human society from potential impacts. NEOs originate in collisions between bodies in the main asteroid belt and have found their way into near-Earth space via complex dynamical interactions. Understanding these interactions, the populations and the orbital element distribution requires accurate orbits and complete samples for the NEO population, in order to properly debias the sample and correctly model the NEO population. Our previous programs of NEO follow-up on the 2-m and 1-m network have tracked and confirmed over a thousand new NEOs, primarily from the Catalina (CSS) and PanSTARRS1 (PS1) surveys. We wish to complement our comprehensive NASA-funded program on the 1-m network to confirm and characterize new NEOs (and comets & Centaurs) discovered by all the feeder surveys, which now includes 100% of PS1, CSS, NEOWISE and an increasing amount from the new PS2 and ATLAS telescopes. Confirming astrometry & photometry for new NEOWISE candidates is particularly important as this IR survey is unbiased to low-albedo objects allowing a cleaner sample but requires the follow-up to confirm NEOs and provide optical fluxes to derive the albedos.

Australian National University

Title PI name Hours (2m) Hours (1m) Hours (0m4)
Surface photometry and distances of newly discovered LSB dwarf galaxies in the constellation of Centaurus Jerjen, H. 40    
Using imaging data from an untargeted shallow survey with the Dark Energy Camera at the 4m Blanco telescope at CTIO we detected a staggering 53 new low-surface brightness dwarf galaxy candidates in the Centaurus A group (D = 4 - 5 Mpc) region, probing the galaxy luminosity function for that environment two magnitudes deeper than ever before. A first list of 16 objects have already been published and a second paper is in preparation. We wish to apply for 50 hours of dark time on the LCOGT 2m telescope at SSO to observe 25 of our best candidates to conduct deeper B, R surface photometry for measuring accurate global parameters such as total magnitudes, effective radii, Sersic indices, color gradients thereby testing their true nature e.g. are they red, gas-poor early-type or blue, star-forming late-type dwarf galaxies. The stacked images should also allow us to measure Surface Brightness Fluctuation (SBF) distances to those objects that were observed under good seeing conditions. The feasibility to measure SBF distances with a 2m class telescope was successfully demonstrated when we used the 2.5m Nordic Optical Telescope at La Palma. Our new measurements will result in the best definition ever of the galaxy luminosity function down to MR = -11 in a specific environment beyond the Local Group. In order to have a statistically representative subsample of the 53 new dwarfs we need to study at least 20-30 objects.
High Precision Photometric Follow-up of HATSouth Planet Candidates Bento, J.   100  
We propose to obtain high precision transit light curves for high priority HATSouth planet candidates. Transiting planets provide unique opportunities for us to understand the properties of exoplanet interior structure, atmospheres, and dynamics. The HATSouth network is the largest ground-based survey for transiting planets, and has already produced six published planets that are suitable for future follow-up studies, as well as over 1000 planet candidates. We will use the LCOGT 1-m network to provide high precision light curves of the transit events of HATSouth planet candidates, these observations will 1) confirm the presence of a planetary transit signal, 2) when combined with other spectroscopic follow-up observations, allow the precise determinations of their system properties, such as planet radius, planet density, planet-star orbital separation, and stellar density. We have shown that the LCOGT 1-m network is perfect for this task, capable of providing high precision light curves, over all longitudes, to measure these time-critical events. We require 100 hours of 1-m time to follow-up 20 high priority planet candidates, these candidates will have been vetted by our observations on the ANU 2.3m telescope, and are the most promising targets from the HATSouth survey.
Transiting Exoplanet CHaracterisation (TECH) Project Bento, J.   30  

ANU contribution to TECH project.

The Next-Generation Sample of Supernovae Yuan, F. 30 35  

ANU contribution to the Supernova key project.

Echo Mapping of AGN Accretion Flows Onken, C. 30 35  

ANU contribution to AGN key project.

Astrophysics Research Institute - Liverpool John Moores University

Title PI name Hours (2m) Hours (1m) Hours (0m4)
The Remarkable Recurrent Novae: Probing their contribution to the SN Ia population Darnley, M. 7 5  
We propose to monitor and follow-up erutpions of Local Group recurrent novae (Rne). Recent studies have gorwn the importance of RNe as Type Ia SN progenitors, by a combination of increased population size and WD mass growth models. Key to studying RNe are the recently uncovered ultra-short recurrence period systems, one in the LMC and two in M31 - including the 6-month duty cycle M31N 2008-12a. These observations will continue to monior eurptions from these systems and the queiscent state, following up new eruptions - in particular the predcited 2016 eruption of M31N 2008-12a. 1m-network bservations of M31N 2008-12a will be used to detect the eruption - triggering follow-up observations from facilities such as HST and XMM, with the 2m-netowrk tasked to follow the eruption itself.
Exploring the bright variable sky Bersier, D. 14    
We propose to obtain photometry and spectroscopy of bright transients detected by the All-Sky Automated Survey for Supernovae (ASAS-SN) that is exploring the bright sky, in the range 12 < V < 17. While the main aim of the project is to find and follow nearby SNe, it is finding numerous other transients. We focus here on supernovae (SNe) and tidal disruption events (TDEs) that will be discovered by ASAS-SN. The high survey cadence means that any transient is found soon after eruption. We will obtain photometry and spectroscopy of SNe and follow their evolution to constrain their progenitors and nucleosynthesis. We have demonstrated very fast turn-around time (few hours) between initial observations and classification and we have a good chance of catching a SN shock breakout. This provides excellent constraints on the radius of the progenitor, hence on its evolutionary status. For TDEs, observations will constrain the mass of the supermassive black hole, the physics of the emission and the total accreted mass. We would use LCOGT facilities for photometry (mostly on 1m telescopes) and spectroscopy (2m telescopes). We have already published papers (most of them include LCOGT data) on different classes of objects, including young stellar objects, AGN, several SNe and three tidal disruption events. We have papers nearing completion for several other SNe and another YSO. We can guarantee that there will be exciting and bright events to follow in any semester. Technical requirements: we expect to use 40% of the time in ToO mode for rapid classification of transients. The rest of the time will be used on 1m telescopes for followup, and some time will be on 2m for classification and late-time followup (when transients have faded beyond the capability of 1m).
Spectro-photometric monitoring of Type Ib/c Supernovae Mazzali, P. 14    
We would like to use the LCOGT network to aid in the work we are currently doing on Type Ib/c Supernovae. We lead the follow-up campaign on the ESO public survey Pessto, and collaborate with iPTF and the Carnegie SN Project. We normally provide 8m telescope time for late phase follow-up, so we would focus on targets that are bright enough to be monitored for 6-12 months. Our proposal would include classical SNe Ib/c, IIb, as well as rarer H-poor transients such as faint & fast events and H-poor SuperLuminous SNe (including Pair Instability candidates). LCOGT instruments give us good coverage in the South, which would be complementary with Pessto (which runs on the ESO-NTT and does not get photometry) and the CSP and add to the LT work in the North, where iPTF is also located. Based on previous experience we may be following 10 SNe per year, and would request some 25 hours per semester, mostly for photometry but including some spectroscopy as well.
Studies of Gamma-ray Bursts and the associated Supernovae Kobayashi, S. 13 7  
We would like to use the LCOGT network to continue the work we have been doing on Gamma-ray bursts, extending it to GRB/SNe. Following triggers from Swift (and sometimes Integral) we can use the LCOGT network (mostly the 2 m telescopes) to monitor GRB light curves. These data are used to build statistical samples, diagnose shock physics and central engine properties possibly determine magnetisation properties for bursts in which reverse and forward shocks can be identified and to determine the GRB light contribution at later time when searching for the contribution from the supernova component in lower redshift objects. If a SN is identified (this requires low-redshift GRBs) we will also follow that both photometrically and spectroscopically, combining LCOGT time with LT/TNG time, in order to determine its properties. The chance to study serendipitous/unique events is also important. We distribute the telescope time across northern and southern telescopes, using both 1 and 2m facilities. Gamma-ray bursts are transient events. We are especially interested in the early afterglow phase (a few mins to a few hrs after GRB triggers) to study shock physics and central engine properties. In order to observe such rapidly fading objects, ToO observations are essential.
Multicolour analysis of blazars Jermak, H.   15  
We propose to undertake U, B, V, R and I photometric monitoring of a sample of 21 blazars (AGN with jets pointed toward observer) to monitor their variability in different wavelengths. We currently have (and continue to take) photometric (and polarimetric) data from the RINGO3 polarimeter on the Liverpool Telescope in three non-standard wavelength bands equivalent loosely to red, green and blue. We want to supplement this ever-growing data set with U, B, V, R and I data from the LCOGT 1-metre telescopes to build a better picture of the colour behaviour of these extremely variable and powerful sources, particularly during flaring/brightening events to explore emission mechanisms. Blazars can be split into subclasses according to the location of the synchrotron peak in their spectral energy distributions (at high-, intermediate- and low- frequencies). We will explore the colour-colour differences between these subclasses in 5 optical filters as we continue our analysis in the 3 RINGO3 wavelength bands.

Chilean Astronomical Community

Title PI name Hours (2m) Hours (1m) Hours (0m4)
Photometric follow-up of planet candidates from the HATSouth project Rabus, M.   150  
The on-going HATSouth project is a wide-field survey searching for transiting extrasolar planets (TEPs) around relatively bright stars. It is producing hundreds of planet candidates per year and it has already announced 17 new planets. In this proposal we request photometric follow-up transit observations of these candidates with 1m-class telescopes. Only this aperture provides enough signal-to-noise for us to take high cadence (2 min) imaging of our candidates and obtain 1-2 mmag precision. This is the level of precision we need for accurate determination of the planetary properties of the systems we uncover. The proposed photometric observations form part of a multi-step strategy for HATSouth follow-up, designed to minimize the use of resources and maximize the confirmed planet yield. The first aim of these photometric observations is to reveal if a given transit-like event has an astrophysical origin and arises from the target star. Additionally, through multi-bandpass observations when possible, we can identify triple system with an eclipsing binary component, which are hidden in the spectrum. The final aim for true exoplanets is to accurately determine their properties.
BLR-size and black hole mass in high-z AGN: Continuation of a very long-term monitoring campaign Lira, P.   5  
Reverberation mapping provides the only tool to determine Black Holes (BH) masses directly, but so far this method has been applied only to small and intermediate systems (L< 1046 ergs/s). We are extending these studies by two orders of magnitude, probing the BH-mass of luminous AGN at redshift 2-3, obtaining the measurement of the largest BHs and extending our knowledge of the physics of AGN and their hosts into the most crucial epoch in galaxy evolution. Since 2005 we have been monitoring 30 very luminous Quasars using broad-band imaging with the 1.3m telescope and in 2007 we started the reverberation campaign of our most variable targets obtaining spectroscopic follow-up with the du Pont telescope.
Accurate Black Hole masses for three southern AGN: key steps to understand accretion physics Lira, P. 13    
Accurate Black Hole masses for three southern AGN: key steps to understand accretion physics
Calibrating the first age-rotation relations for Gyr old field stars using wide binaries Chaname, J.   60  
Calibrating the first age-rotation relations for Gyr old field stars using wide binaries
Characterizing ASAS-SN Transients: Physical Properties, Progenitors, Distances, and Rates Prieto, J.   60  
Characterizing ASAS-SN Transients: Physical Properties, Progenitors, Distances, and Rates
TAROT-LCOGTN multi-band photometric monitoring of short-period binaries showing evidence of chromospheric activity Mennickent, R.     60
TAROT-LCOGTN multi-band photometric monitoring of short-period binaries showing evidence of chromospheric activity

Faulkes Telescope Project - Cardiff University

Title PI name Hours (2m) Hours (1m) Hours (0m4)
LMXB Monitoring Lewis, F. 60 20  
Monitoring of LMXBs as documented at faulkes-telescope.com/XRB. Continued monitoring of approx 40 transient/quiescent sources.
Education - On Sky Roche, P. 40 10  
Use of On Sky for FTP education program.
Education - Queue observations Roche, P. 200 180  
Use of queue observations for FTP education program.

Instituto de Astrofisica de Canarias

Title PI name Hours (2m) Hours (1m) Hours (0m4)
Follow-up of primary eclipses of a benchmark stellar triple system Alonso, R.     100
Follow-up of primary eclipses of a benchmark stellar triple system
VRIHα followup of Be Xray binary systems from Siding Spring (Australia) Blay, P.     25
VRIHα followup of Be Xray binary systems from Siding Spring (Australia)
SHAPE, POLE, SIZE, ALBEDO AND THERMAL INERTIA OF CYBELE AND HILDA Licandro, J.     100
SHAPE, POLE, SIZE, ALBEDO AND THERMAL INERTIA OF CYBELE AND HILDA
Photometric monitoring of the M dwarfs in the Carmenes sample: the Barnard star Bejar, V.     120
Photometric monitoring of the M dwarfs in the Carmenes sample: the Barnard star
COBIPULSE-SOUTH: A systematic search for compact binary pulsars Linares, M.     55
COBIPULSE-SOUTH: A systematic search for compact binary pulsars

University of Hawaii - Institute for Astronomy

Title PI name Hours (2m) Hours (1m) Hours (0m4)
HI STAR Projects Armstrong, JD 45 45 60
The Hawaii Student Teacher Astronomy Research program (HI STAR) is a week long summer program for middle and high school students. At the summer program students work with mentors on starting a research project which the students will continue through the year. The goal ot the HI STAR program is to have students conduct astronomy research projects, enter their projects in the science fair, and eventually major in science, engineering, or technology when they go to college. Typical student research projects include variable stars; asteroid recovery, rotation, and color; exoplanets; galaxies; etc. While this is an EPO program the students are conducting research and some students may submit peer reviewed papers on their research so a proprietary period is desirable.
HI STAR Projects II Armstrong, JD 45 45 60
The Hawaii Student Teacher Astronomy Research program (HI STAR) is a week long summer program for middle and high school students. At the summer program students work with mentors on starting a research project which the students will continue through the year. The goal ot the HI STAR program is to have students conduct astronomy research projects, enter their projects in the science fair, and eventually major in science, engineering, or technology when they go to college. Typical student research projects include variable stars; asteroid recovery, rotation, and color; exoplanets; galaxies; etc. While this is an EPO program the students are conducting research and some students may submit peer reviewed papers on their research so a proprietary period is desirable.
Astro 301 Armstrong, JD 10 10 20
Students at the University of Hawai'i Manoa Astronomy 301 research class will be performing authentic astronomical research. Observations will be collected to support these activities.
0m4 educational data sets Armstrong, JD     60
0m4 educational data sets

National Astronomical Observatories of China

Title PI name Hours (2m) Hours (1m) Hours (0m4)
Constraining Free-Floating Planets in the Galaxy Mao, S.   50  
NAOC contribution to Microlensing key project.
Multi-band Photometric Monitoring of Extragalactic Transients Discovered by ASAS-SN Dong, S.   70  
We are in a golden era of time-domain astronomy, with several optical transient surveys finding hundreds of sources per year. However, most of these transients are poorly studied due to their relative faintness and lack of follow-up resources. Here we propose to use the LCOGT 1m telescopes to obtain multi-band and well-sampled light curves of a complete sample of nearby extragalactic transients (discovery magnitude V <~ 17 mag, D <~ 200 Mpc), mainly supernovae, that will be selected from the ASAS-SN surveys. The well-sampled light curves obtained with this program will be used to characterize the physical properties of the explosions (e.g., source of the emission, radiated energies, ejecta and 56Ni masses, dust formation) and for constraining their progenitor stars and explosion mechanisms. For Type Ia and Type IIP supernovae, these data will also be used to obtain accurate distances. To augment our high-cadence photometry, we will obtain spectral time-series of the targets via coordination with a several mid-sized telescopes available to us.
Observations of Young Supernovae for Precision Cosmology Wang, X.   60  
NAOC contribution to Supernova key project.
LCOGT photometric measurements of new classical Cepheids in the northern Galactic disk de Grijs, R.   20  
LCOGT photometric measurements of new classical Cepheids in the northern Galactic disk

South African Astronomical Observatory

Title PI name Hours (2m) Hours (1m) Hours (0m4)
AGN Reverberation (Echo) Mapping Romero-Colmenero, E.   60  
SAAO contribution to AGN Echo Mapping Key Project
The Next Generation Sample of Supernovae Kasai, E.   50  
SAAO contribution to Supernova Key Project
Transiting Exoplanet CHaracterisation (TECH) Project Sefako, R.   50  
SAAO contribution to TECH Project
Time-domain astrophysics of magnetic CVs, continued Potter, S.   60  
Magnetic CV (mCV) research has been an unofficial key SAAO/UCT research programme for the past ~ 3 decades. In that time we have built up expertise in high time domain photometry, spectroscopy and polarimetry of mCVs. Presently we have multiple on-going active observing campaigns using the SALT, SAAO small telescopes and other Gamma and X-ray observatories through international collaborations. This proposal has two main objectives. The first is to boost the scientific output of our ongoing campaigns by providing up-to-date light curves and to provide timely notification of infrequent or rare extreme events (targets of opportunity). Secondly, to extend our time-domain exploration of mCVs to the longer time domain in order to address our lack of knowledge and understanding of the long term physical accretion processes of mCVs.
Optical ToO observations with LCOGT for H.E.S.S. van Soelen, B.   33  
The H.E.S.S. gamma-ray telescope regularly partakes in campaigns to obtain multi-wavelength observations of variable very-high-energy (VHE: E > 100 GeV) ?-ray sources. Here we propose for ToO time on the LCOGT system to provide optical support for such coordinated multiwavelength observations. The most probable targets will be extra-galactic sources such as blazars and GRBs. Blazars display rapid variability across all wavelengths and while some studies have found tight correlations between the optical, X-ray and gamma-ray emissions, others have not. Observed correlations (or lack thereof), which often include more complicated patterns than simple linear flux-flux correlations, place constraints on the particle acceleration and radiation mechanisms at work within these systems. A major part of the science being undertaken with the H.E.S.S. II telescope is the attempted VHE gamma-ray detection of a GRB. While GRBs are routinely observed at MeV energies and have been detected up to 95 GeV by Fermi-LAT, so far none has been detected at energies above 100 GeV. The H.E.S.S. II telescope has a fully automated GRB observation system, automatically repositioning the system for prompt follow-up observations of GRBs, within as short as 60 seconds, without the need for intervention by the observation shift crew. The LCOGT provides a unique resource to allow for simultaneous optical and VHE observations.
Light-Curve of Possible Super-AGB Stars in NGC 6822 Whitelock, P.   2  
We propose obtaining one exposure per month in the RCband of the hot bottom burning (HBB) variables in IC 1613 in order to characterize their variability and in particular to find out if the period of the lithium-rich star is changing. Such a change could indicate that it is undergoing real-time evolution.
Study photometric structure of southern lenticular galaxies in clusters Kniazev, A.   43  
The goal of the project is to study photometric structure of southern lenticular galaxies in clusters. The project supplements the spectral program is now active at SALT. To attribute the stellar population ages and metallicities measured along the slit of spectrograph to certain large-scale components of the galaxies studied, we need the images in gri bands. After data obtaining, we will decompose observed galaxies into bulges and disks to determine strict radial borders and relative brightness contributions of the components at different radii.
Confirming the LBV status of spectroscopically selected LBV candidates Kniazev, A.   10  
none.
Evolutionary Period Changes in Hot Bottom Burning Stars? Menzies, J.   3  
none.
Observations of stellar occultations by large trans-Neptunian Objects Sickafoose, A.   15  
none.

Scottish Universities Physics Alliance

Title PI name Hours (2m) Hours (1m) Hours (0m4)
Exploring Cool Planets Beyond the Snow Line Street, R.   1550  
SUPA contribution to Microlensing Key Project
Echo Mapping of AGN Accretion Flows Horne, K. 75 250  
SUPA contribution to AGN Echo Mapping Key Project
Transiting Exoplanet CHaracterisation (TECH) Project Bayliss, D.   100  
SUPA contribution to TECH project.
Transiting Exoplanets Cameron, A.   100  
Follow-up of transiting extrasolar planet candidates identified in ground-based surveys (e.g. WASP,QES).
Time-Domain Observations of Young Stellar Objects (TOYS) Scholz, A.   50  
Young stellar objects show variability on a range of timescales, caused by a variety of physical mechanisms. Some of them are periodic and associated with stellar and disk rotation, others are irregular and based on instabilities. We want to use LCOGT 1-m time to carry out multi-filter monitoring of ~100 YSOs to a) map their (stable) circumstellar environment (hot spots, inner disk bubbles, disk clumps), b) to measure timescales/frequencies for instabilities, and c) to identify specific objects for follow-up with larger telescopes. We plan to focus on one star forming region per semester - Chamaeleon-I in April/May and SigmaOri in November/December. With the Sinistro detectors, the field of view will cover several dozen known and well-characterised YSOs in each region. The regions can be covered almost 24/7 with the 1-m network during these months.
Science from GAIA Alerts Dominik, M.   80  
Follow-up of e.g. GAIA transients.

Tel Aviv University: Israeli Center Of Research Excellence

Title PI name Hours (2m) Hours (1m) Hours (0m4)
Black Holes in binary systems in the LMC Mazeh, T. 175    
Black Holes in binary systems in the LMC
Companions and debris around white dwarfs Maoz, D. 75 100  
Companions and debris around white dwarfs
Low surface brightness tidal features around interacting galaxies Brosch, N. 0 0  
Low surface brightness tidal features around interacting galaxies

University of Texas

Title PI name Hours (2m) Hours (1m) Hours (0m4)
Measuring the Spin-Orbit Misalignment of a Young Substellar Binary: Simultaneous Photometry Johnson, M.   8  
Measuring the Spin-Orbit Misalignment of a Young Substellar Binary: Simultaneous Photometry
Candidate Planets in the Upper Scorpius Star Forming Region Mann, A.   36  
Candidate Planets in the Upper Scorpius Star Forming Region
Supernova Light Curves with the LCOGT SN Key Project Cochran, W.   50  
U. Texas contribution to Supernova Key Project
Transiting Exoplanet CHaracterisation (TECH) Project Wheeler, J.   50  
U.Texas contribution to TECH Project

University of Heidelberg

Title PI name Hours (2m) Hours (1m) Hours (0m4)
Gaia Tracking Altmann, M. 10    
Tracking of the GAIA spacecraft as part of the Ground-Based Optical Tracking (GBOT).
Heidelberg AGN Monitoring Wambsganss, J.   100  
Heidelberg AGN Monitoring

NYU, Abu Dhabi

Title PI name Hours (2m) Hours (1m) Hours (0m4)
NYU, Abu Dhabi research and education Roberts, M. 37 65  
 

Nanjing University

Title PI name Hours (2m) Hours (1m) Hours (0m4)
Quasar Variability Shi, Y.   250  
Quasar Variability

SouthWest Research Institute

Title PI name Hours (2m) Hours (1m) Hours (0m4)
Asteroid Light Curve Photometry Buie, M.   150  
Asteroid Light Curve Photometry

Queens University Belfast

Title PI name Hours (2m) Hours (1m) Hours (0m4)
Public ESO Spectroscopic Survey of Transient Objects (PESSTO) Follow-up Observations Smartt, S.   50  
Public ESO Spectroscopic Survey of Transient Objects (PESSTO) Follow-up Observations

The Ohio State University

Title PI name Hours (2m) Hours (1m) Hours (0m4)
Photometric Follow-up of ASAS-SN Transients Stanek, K.   50  
Photometric Follow-up of ASAS-SN Transients