Poster Abstracts
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1. John Baker ( NASA-GSFC )
Co-authors: Jeremy SchnittmanTitle: Building a toolkit for Bayesian analysis of WFIRST microlensing capability.
Abstract: The WFIRST microlensing survey will provide unprecedented capability to gravitationally observe the small and/or dark objects crossing between us and the stars in the central part of the galaxy. While the mission focuses on identifying planetary systems, many events will involve other objects including stellar binaries, dwarf stars, and dark compact objects. Unlike groundbased observation, WFIRST will have both high-precision photometric and astrometric channels for lensing observations, and at high cadence. Combining these channels will provide new opportunities for breaking lens model degeneracies, allowing detailed parameter measurements, but will also require a vigorous systematic approach to data processing. We discuss early steps toward developing a Bayesian analysis tool set for studies of WFIRST capability.
2. Andrew William Blain ( University of Leicester )
Co-authors: Carrie Bridge (Caltech); Peter Eisenhardt (JPL); Suzy Jones (Leicester); Carol Lonsdale (Virginia); other WISE team members.Title: Overdensities of sub millimeter galaxies around WISE-selected AGNs
Abstract: Surveys using the 850-micron SCUBA2 camera at the JCMT have found over densities of emitting objects throughout 3-arcmin-diameter regions around WISE-selected mid-IR-luminous AGNs. The over densities exceed the field galaxy density by factors of 2.5 for WISE-color-selected "HotDOGs" and by 5 for WISE-radio-selected objects. I will describe the results of the observations for the SEDs of the WISE-selected galaxies, and for the properties of their environments.
3. Denis Burgarella ( Laboratoire d'Astrophysique de Marseille )
Co-authors: Denis Burgarella (LAM); Kjetil Dohlen (LAM); Sébastien Vives (LAM); Toru Yamada (Tohoku/JAXA); Ikuru Iwata (NAOJ); Giovanni Fazio (SAO/CfA); Marcin Sawicki (St.Mary's); and WISH TeamTitle: WISH Spec: a 1-arcmin 1-5um IFU for the Wide-field Infrared Surveyor for High-redshift
Abstract: WISH (Wide-field Infrared Surveyor for High-redshift) is a space science mission concept whose primary goal is to study the first galaxies in the early universe. WISH will conduct unique ultra-deep and wide-area sky surveys in the wavelength range 1-5 micron. In addition to the imaging focal plane, a spectroscopic parallel-mode spectrograph (WISH-Spec, Integral-Field Unit) in the same Near-IR range is planned. WISH-Spec is studied in Europe under the responsibility of LAM. Although the instrument design is still open, with the parallel mode, we could envisage very deep exposure times in spectroscopy over (relatively) wide areas. In this talk, we will first present the characteristics of the instrument itself. Next, we will present the unique science that can be carried out from the spectrograph to physically study galaxies at 3 < z < 9 and try to address the question: "How did the Universe originate and what is it made of?". An important point that we will also discuss is the similarities and differences of WISH-Spec with other spectrographs in the NIR (JWST, ELTs, EUCLID, WFIRST).
4. Yi-Kuan Chiang ( University of Texas at Austin )
Co-authors: Roderik Overzier; Karl GebhardtTitle: The Rise of Galaxy Clusters at z~2 in the Previrialization Epoch
Abstract: The WFIRST grism survey has enormous potential for studying galaxy cluster formation during the epoch at z ~ 2 before virialization erased the signatures of the rapid mass assembly and galaxy growth. I will present my work on cosmological simulations of cluster formation (Chiang et al. 2013) as well as new evidence for a wide range of high redshift overdensities (protoclusters) in the COSMOS field (Chiang et al. 2014). In particular, the distribution of photo-z and Lya-selected galaxies (LAEs) in the region of COSMOS covered by the HETDEX Pilot Survey (HPS), shows a large concentration at z = 2.44. The high overdensity of galaxies (and dark matter) in this region is reflected by a large volume overdensity in stellar mass. This structure will collapse to form a galaxy cluster with ~10^14.5 M_sun by z = 0. The structure is also seen in the form of a large-scale enhancement of Lyman-alpha absorbing gas (Lee et al. 2014), demonstrating the synergy of these independent techniques for identifying highly overdense regions at high redshift. The structure also hosts several extended Lya halos (>~ 60 kpc), some of which are identified as AGN in the X-ray. These systems are commonly found in overdense regions at high redshift, perhaps indicating the accelerated co-evolution of massive galaxies and their supermassive black holes in overdense environments. WFIRST will provide large samples of such galaxy concentrations, allowing a better understanding of the interplay between cluster formation, star formation, and black hole accretion.
5. James William Colbert ( IPAC )
Co-authors: Jeffrey Kruk; Lee Armus; Gabriel Brammer; Stefano Casertano; Roc Cutri; Van Dixon; Alaina Henry; Davy Kirkpatrick; John MacKenty; Marc Postman; Swara Ravindranath; Harry Teplitz; Roeland van der MarelTitle: WFIRST Grism Simulations
Abstract: We present preliminary grism simulations for the WFIRST space mission. We take fields observed by the Hubble Space Telescope WFC3 grism and then apply the pixel scale, throughput, wavelength resolution, and spectral sensitivity of the planned WFIRST grism to generate simulated images. We simulate the same fields at several different roll angles to better examine the potential issues of contamination and spectral overlap. We briefly discuss planned future simulation improvements.
6. Patrick Cote ( NRC Herzberg Astronomy and Astrophysics )
Co-authors: M. Balogh (Waterloo); R. Carlberg (Toronto); L. Drissen (Laval); J. Dupuis (CSA); W. Fraser (NRC-Herzberg); J. Hutchings (NRC-Herzberg); JJ. Kavelaars (NRC-Herzberg); D. Laurin (CSA); C. Robert (Laval); M. Sawicki (St. Mary's); A. Scott (COM DEV); R. Sorba (St. Mary's); L. Van Waerbeke (UBC);Title: The CASTOR Mission Concept: Scientific Opportunities in the Era of Wide-Field Infrared Surveys
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Abstract: The "Cosmological Advanced Survey Telescope for Optical and uv Research" (CASTOR) is a proposed wide-field blue-optical/UV imaging telescope that is being investigated by the Canadian Space Agency. The nearly diffraction-limited 1m CASTOR telescope would perform deep, panoramic imaging in three filters covering the ultraviolet and blue-optical spectral regions (0.15-0.55 microns) at a spatial resolution comparable to the Hubble Space Telescope but with a roughly 200-fold gain in field of view. In this talk, I will summarize the status of the proposed mission, including ongoing technical work on the focal plane array and optomechanical design, and highlight the potential synergies with WFIRST, Euclid and LSST.
7. Yu Dai ( Caltech-IPAC )
Co-authors: Harry Teplitz; Matt Malkan; James Colbert; Marc Rafelski; Claudia Scarlata; Micaela Bagley; Alaina Henry; Nate RossTitle: The power of infrared grism spectroscopy survey
Abstract: We present the results of the HST/WFC3 Infrared Spectroscopic Parallel (WISP) Survey, which probes galaxy evolution with infrared grism spectroscopy. This space-based survey covers a broad, continuous spectral range of 0.8--1.7 um, and has measured the redshifts of thousands of low-mass, metal-poor galaxies and galaxies with extreme star formation rates (SFR). Majority of the newly discovered galaxies reside in 0.5 < z < 2.5, a redshift desert difficult to observe with the ground-based continuum-selected surveys. With the power of the WISP survey, we studied the de-reddened SFR and mass relations, the mass-metallicity relation at z > 1 especially at low mass ends; the ages of absorption-line galaxies down to J=24-25; and special objects like metal poor dwarfs and extreme starbursts, Lyman alpha emitters at z > 6 and galaxy pairs.
8. Michael A DiPompeo ( University of Wyoming )
Co-authors: Adam Myers; Ryan Hickox; Jim Geach; Gil Holder; Kevin Hainline; Jo BovyTitle: IR Quasar Selection and CMB Lensing Correlations
Abstract: The infrared provides powerful constraints on quasar selection, especially for those that are optically obscured by gas and dust. By incorporating NIR and MIR data into probabilistic quasar selection techniques, we can drastically improve methods that have previously relied on optical data alone. These probabilistic techniques are also both more complete and efficient than simple IR color cuts that have recently been used to select quasars from Spitzer and WISE data. These large photometric quasar samples allow us to study them with the new and powerful method of cross-correlations with CMB lensing maps. We have recently used WISE-selected samples split into obscured and unobscured populations and CMB lensing maps from Planck to demonstrate the power of these cross-correlations to study quasar subsamples. WFIRST will be a critical tool to continue developing IR quasar selection techniques and study the obscured population.
9. Van Dixon ( STScI )
Co-authors: C. J. Willott (NRC Herzberg Institute of Astrophysics; Canada)Title: Simulating Wide-Field Slitless Spectroscopy with JWST/NIRISS
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Abstract: The Near Infrared Imager and Slitless Spectrograph (NIRISS) aboard the James Webb Space Telescope (JWST) will offer wide-field slitless spectroscopy (WFSS) with a resolving power R = 150 at wavelengths from 0.8 to 2.25 microns. In this band, NIRISS is sensitive to Lyman-alpha emission lines and continuum breaks in the spectra of galaxies with redshifts between 6 and 17, allowing it to probe the first stars and ionizing sources in the early universe. We have modeled a NIRISS observation of the massive galaxy cluster MACS J0647+7015. Using images, photometry, and redshifts from the CLASH survey, we constructed a series of simulated direct and dispersed images in the six filters used for WFSS with NIRISS. We present the results of this analysis and discuss their implications for the ability of NIRISS to detect and parameterize high-redshift galaxies in crowded fields. NIRISS is provided to the JWST project by the Canadian Space Agency under the leadership of René Doyon of the Université de Montréal. The prime contractor is COM DEV Canada.
10. Keigo Enya ( JAXA/ISAS )
Title: Technologies for infrared coronagraphs for space-borne telescopes
Abstract: Based on public information, this poser reviews technologies for infrared coronagraphs developed for space-borne telescopes. Though the SPICA Coronagraph Instrument (SCI) was dropped in the drastic change of whole of the mission, developed technologies have potential to be useful for coronagraphs for space-borne telescopes. Design, fabrication, and experiments of shaped pupil mask coronagraph for obscured pupils, highly stable vacuum chamber, optics for wavefront correction, and others are shown.
11. Taran LeRoy Esplin ( Penn State )
Co-authors: Kevin Luhman; Eric Mamajek; Elijah MillerTitle: A WISE Survey of Circumstellar Disks
Abstract: Complete samples of circumstellar disks in star-forming regions and accurate classifications of those disks represent a foundation for studies of star and planet formation. Using data from the Wide-field Infrared Survey Explorer All-Sky Release Catalog and other catalogs of ancillary data, we have searched for new members in the Taurus and Upper Sco star-forming regions by identifying sources with red mid-infrared colors. While we have identified many candidates, membership confirmation requires follow-up spectroscopy. The WFIRST mission will provide an efficient method for confirming candidates and allow for the completion of disk-bearing member censuses of star-forming regions.
12. Michael Florian ( University of Chicago )
Co-authors: Nan Li; Michael Gladders; Salman Habib; Katrin Heitmann; Keren Sharon; Matthew Bayliss; Jane RigbyTitle: The Gini Coefficient and Strong Lensing: Measuring Morphology in Strongly Lensed Galaxies
Abstract: WFIRST-AFTA will discover 1000s of new strong lensing systems. Even with current samples of 10s to 100s, the bottleneck to empirically contetxualizing the lensed sources with respect to the general high-z galaxy population is the apparent requirement of lens mass modeling, needed to build images of the lensed sources in the source plane. This problem will only get worse as samples become larger. We have thus been actively seeking observables that are invariant under the typical strong lensing transformations. One such galaxy observable is the Gini coefficient, a measure of the inequality in the distribution of light in a galaxy which has previously been used successfully in morphological studies of unlensed galaxies. We demonstrate through simulations that the Gini coefficient is only very weakly affected by the transformations of strong gravitational lensing. We also present results of Gini coefficient measurements on a sample of ~50 lensed galaxies with redshifts between 1 and 5.
13. Ori Fox ( UC Berkeley )
Title: Infrared Follow-up Observations of Supernovae in the WFIRST Era
Abstract: Despite significant progress in the SN field over the past few years, infrared (IR) observations of SNe remain sparse. The lack of data is further perpetuated by the dearth of both easy access to IR instrumentation and mid-IR wavelength coverage. While 25-m+ telescopes may not offer “easy-to-access” IR capabilities, they will coincide with JWST, WFIRST, and an ever-expanding suite of IR instruments. Here I describe some of the key topics that will probed by the next generation of IR observations of SNe, and the role large, ground-based telescopes can play.
14. Kevin Nicholas Hainline ( Dartmouth College )
Co-authors: Ryan C. Hickox (Dartmouth College); Christopher M. Carroll (Dartmouth College); Adam D. Myers; Michael A. DiPompeo (University of Wyoming); Laura Trouille (Northwestern University; Adler Planetarium)Title: A Spectroscopic Survey of WISE-selected Obscured Quasars with the Southern African Large Telescope
Abstract: In this poster, we present the results of an optical spectroscopic survey of a sample of 40 candidate obscured quasars identified on the basis of their mid-infrared emission detected by the Wide-Field Infrared Survey Explorer (WISE). Optical spectra for this survey were obtained using the Robert Stobie Spectrograph (RSS) on the Southern African Large Telescope (SALT). Our sample was selected with WISE colors characteristic of AGNs, as well as red optical to mid-IR colors indicating that the optical/UV AGN continuum is obscured by dust. We obtain secure redshifts for the majority of the objects that comprise our sample (35/40), and find that sources that are bright in the WISE W4 (22 micron) band are typically at moderate redshift (<z> = 0.35) while sources fainter in W4 are at higher redshifts (<z> = 0.73). The majority of the sources have narrow emission lines, with optical colors and emission line ratios of our WISE-selected sources that are consistent with the locus of AGN on the rest-frame g-z color vs. [NeIII]3869 / [OII]3726+3729 line ratio diagnostic diagram. We also use empirical AGN and galaxy templates to model the spectral energy distributions (SEDs) for the objects in our sample, and find that while there is significant variation in the observed SEDs for these objects, the majority require a strong AGN component. Finally, we use the results from our analysis of the optical spectra and the SEDs to compare our selection criteria to alternate criteria presented in the literature. These results verify the efficacy of selecting luminous obscured AGNs based on their WISE colors, and show the importance of future near-IR imaging and spectroscopy of obscured quasars with WFIRST-AFTA.
15. Rene Hudec ( CTU in Prague & AI AS CR Ondrejov )
Co-authors: V. Tichy; L. Pina; A. InnemanTitle: Lobster Eye X ray WF Survey and synergy with IR
Abstract: Multispectral analysis represents important technique in modern astrophysics. I will introduce novel methods for wide field X ray surveys based on innovative Lobster Eye Monitors and will discuss the synergy between these and IR surveys.
16. Rene Hudec ( CTU in Prague & AI AS CR Ondrejov )
Co-authors: V. Tichy; L. HudecTitle: IR sky surveys with ESA satellite Gaia and photographic data archives
Abstract: We will introduce and discuss the IR survey provided by the ESA Gaia satellite and by photographic sky surveys (icluding IR) in the past which after digitization represent valuable astrophysical data source aas well. The emphasis will be given on very Low Dispersion Spectroscopy (LDS) and its application in modern astrophysics including high-z universe.
17. Kevin Huffenberger ( Florida State University )
Co-authors: K. Huffenberger; T. Diamond; P. Hoeflich; D. Collins; D. Rubin; & FSU Astro groupTitle: Type Ia Supernovae: Probing the Diversity and Evolution with Redshift
Abstract: Type Ia Supernovae are an essential tool for cosmology and understanding the origin of elements. Although a two-parameter color/decline-rate correction allows their cosmological use with present numbers of supernovae, precision observations show much more diversity in spectra and as secondary light-curve parameters. This diversity demands a better understanding of the wide range of physics which includes progenitor systems, nuclear burning, hydrodynamics and, possibly, magnetic fields. Observations are needed to narrow the range of possible scenarios and their frequency realized in nature. Based on detailed calculations for explosions, light curves and spectra, we present two methods: differential analysis of optical light curves to probe the progenitors, and IR line profiles at late times (namely the forbidden [FeII] at 1.644 micron). Both methods would allow us probe the diversity of explosion physics and progenitors. However, the IR-profiles put many more additional, independent constrains on the physics such as the magnetic fields, total mass, and hydrodynamical mixing. We tested both methods on SN 2005df and SN 2014J and found consistent results. However, larger samples and higher accuracy, approximately 1-5 %, in line profiles are required to ensure we have an adequate understanding of the population and underlying physics. We suggest using the unique spectroscopic capabilities of WFIRST to probe the IR line profiles up to a redshift of about z ~ 0.2 to limit the physical parameter space, test and calibrate the optical light curve method, and ensure that rest-frame optical will adequately control population drift.
18. Akio K Inoue ( Osaka Sangyo University )
Co-authors: Ikkoh Shimizu (Tokyo U.); Naoki Yoshida (Tokyo U.); Takashi Okamoto (Hokkaido U.)Title: UV/Optical/IR nebular emission lines from high-z LBGs
Abstract: We will present an expectation of nebular emission line fluxes from high-z LBGs detected with future wide-field near-infrared surveys. Based on a state-of-the art cosmological galaxy formation simulation, we have made a large mock catalogue of realistic LBGs at z>6. With a nebular emission line model by Inoue (2011), we have calculated emission line fluxes from each LBG in the catalogue. We will discuss the feasibility of the emission line detection by follow-up spectroscopy with TMT, JWST, and ALMA.
19. Woong-Seob Jeong ( Korea Astronomy & Space Science Institute )
Co-authors: Woong-Seob Jeong(1,2); Jeonghyun Pyo(1); Toshio Matsumoto(1,3,4); Il-Joong Kim(1); Won-Kee Park(1); Dae-Hee Lee(1); Bongkon Moon(1); Sung-Joon Park(1); Youngsik Park(1); Duk-Hang Lee(1,2); Ukwon Nam(1); Minjin Kim(1); Jongwan Ko(1); Jeong-Eun Lee(5); Myungshin Im(6); Hyung Mok Lee(6)(1) KASI; Korea; (2) UST; Korea; (3) ASIAA; Taiwan; (4) ISAS/JAXA; Japan; (5) KHU; Korea; (6) SNU; Korea
Title: Korean Activities of Infrared Space Missions
Abstract: We review Korean activities in infrared space missions. After the successful collaboration in Japanese infrared space mission, AKARI, the importance of space infrared observation led Korean astronomical society to develop the Korean infrared missions. Since the small satellite series are the unique programs for the space science in Korea, most of scientific objectives are focused on diffuse objects. One of major targets is the measurement of Cosmic Infrared Background (CIB) which gives us to understand indirectly distant galaxy/star populations and their formation and evolution in early Universe. The observation of CIB in space is essential due to its very week brightness and fluctuation. We designed the near-infrared space telescopes optimized to the observation of CIB for small satellite. After the successful launch of MIRIS (Multi-purpose InfraRed Imaging System) last year, MIRIS have performed the CIB observation to measure its degree-scale fluctuation in two wide bands (I and H band). Based upon the heritages from MIRIS, the Near-infrared Imaging Spectrometer (NISS) have being developed. The NISS will carry out the near-infrared imaging spectroscopic observation, which supplies us the spectral variation of the CIB fluctuation.
20. Rubab Khan ( NASA/GSFC )
Co-authors: K. Z. Stanek; C. S. KochanekTitle: An Emerging Class of Extragalactic Self-Obscured Stars
Abstract: The evolution of the most massive stars such as η Carinae is controlled by the effects of mass-loss. Understanding these stars is challenging because no true analogs of η Car have been clearly identified in the Milky Way or other galaxies. Copious mass-loss leads to circumstellar dust formation, obscuring the star in the optical. But as the light is re-emitted by the dust, these objects become very luminous in the mid-IR. We have carried out a systematic search for η Car analogs in 7 galaxies, utilizing data from Spitzer, Herschel, HST and other sources. Our search detected no true analogs of η Car, however, we do identify a significant population of 18 lower luminosity (log(L/L_⊙)∼eq5.5-6.0) dusty stars. Stars enter this phase at a rate that is a fraction 0.09 ≲ F ≲ 0.55 of the ccSN rate, and this is consistent with all 25~<~M_{ZAMS}~<~60M_⊙ stars undergoing an obscured phase at most lasting a few thousand years once or twice. These phases constitute a negligible fraction of post-main sequence lifetimes of massive stars, which implies that these events are likely to be associated with special periods in the evolution of the stars. The mass of the obscuring material is of order ∼ M_⊙, and we simply do not find enough heavily obscured stars for these phases to represent more than a modest fraction (∼ 10% not ∼ 50%) of the total mass lost by these stars. While this search has been feasible using archival Spitzer data, JWST will be a far more powerful probe of these stars. The HST-like resolution of JWST will either greatly reduce the problem of confusion or greatly expand the possible survey volume. Far more important will be the ability to carry out the survey at 24 μm, which will increase the time over which dusty shells can be identified from hundreds of years to thousands of years, greatly improving the statistics and our ability to survey the long term evolution of these systems and the relationship between stellar eruptions and supernovae.
21. Minjin Kim ( KASI (Korea Astronomy and Space science Institute) )
Co-authors: Woong-Seob Jeong; Jeonghyun Pyo; NISS teamTitle: The Science Cases for Near-infrared Imaging Spectrometer for Star formation history (NISS)
Abstract: We present science cases for a small space telescope - Near-infrared Imaging Spectrometer for Star formation history (NISS) onboard NEXTSat-1 (Next generation of small Satellite) in Korea. The NISS is a near infrared (NIR) imaging spectrometer mounted to telescope with an aperture of 15 cm, that will be launched on 2017. It has a field of view of 2 by 2 deg and covers from 0.9 to 3.8um with a spectral resolution of 20, which is high enough to estimate strength of various emission lines from star forming regions and active galactic nucleus. The dataset from NISS will allow us to study cosmic star formation history of galaxies in nearby and distant universe through physical properties of star forming region in our galaxy as well as nearby galaxies and the structure evolution of fluctuation from cosmic infrared background in distant time scale.
22. Jongwan Ko ( Korea Astronomy and Space Science Institute (KASI) )
Title: Tracing recent star formation of massive early-type galaxies
Abstract: We study the mid-infrared (IR) and near-ultraviolet (UV) excess emissions of early-type galaxies (ETGs) on the optical red-sequence at z < 1 using a spectroscopic sample of galaxies in the Sloan Digital Sky Survey (SDSS) Data Release 7 and in the fields of Great Observatories Origins Deep Survey (GOODS). In the mass-limited GOODS sample of 1025 galaxies with M_star > 10^10.5 M⊙ and 0.4 < z < 1.05, we identify 696 Spitzer 24 μm detected (above the 5σ) galaxies and find them to have a wide range of rest-frame NUV-r and r-[12 μm] colors despite their red optical u−r colors. The combination with the results of SDSS red ETGs in the local universe suggests that the recent star formation is not rare among quiescent, red ETGs at least out to z ~1 if the mid-IR excess emission results from intermediate-age stars or/and from low-level ongoing star formation.
23. Tadayuki Kodama ( NAOJ )
Co-authors: SWIMS-18 team and WISH-7 teamsTitle: Super multicolor wide-field NIR imaging surveys (SWIMS-18 and WISH-7)
Abstract: We are planning to conduct an unprecedentedly large multi-band NIR survey called SWIMS-18 on Subaru and eventually on a 6.5m telescope TAO (Tokyo Atacama Observatory). We have manufactured a large set of 9 medium-band and 6 narrow-band filters as well as 3 broad-band filters (18 filters in total) on a new NIR wide-field instrument SWIMS. The great efficiency with dual channel simultaneous observations that its dichroic mirror offers, and a large telescope time available, we will conduct a designated large survey of distant galaxies in the redshift interval of 1<z<5 (at rest-frame optical). The dual emitter search (Ha and [OIII]) with 4 pairs of NB filters is also absolutely unique and will deliver information on ionization state of individual galaxies. SWIMS-18 survey will thus expand the current survey volume by a factor of >>10 and construct the largest homogeneous NIR selected sample of distant galaxies which forms the basis of TMT targets. We also plan to extend this concept to even higher redshifts (2.8<z<6.6 for Ha and 4<z<9 for [OIII]) with WISH space telescope, again having Ha/[OIII] pair filters. This will enable us to go all the way back in time to step into the reionization epoch.
24. Nanyao Lu ( NHSC/IPAC, Caltech )
Co-authors: Nanyao Lu; Y. Zhao; C. Xu; T. Diaz-Santos; L. Armus; J. Mazzarella; J. Howell (IPAC/Caltech); Y. Gao (PMO) (for the GOALS-SPIRE/FTS Team)Title: Measuring the Star-formation Rate and its Surface Density in High-z Galaxies Using CO(7-6) and [NII] 205 um Lines
Abstract: To fully characterize the global star formation (SF) activity in a high-z galaxy, one needs to know not only the overall star formation rate (SFR), which drives the total IR luminosity L(IR), but also its effective SF surface density, which drives the far-infrared (FIR) color, C(60/100), of the dust continuum emission. We show for the first time that this can be accomplished by measuring the fluxes of just two spectral lines, CO(7-6) at 372 um and [NII] at 205 um. Using local (ultra) luminous infrared galaxies [(U)LIRGs], we show that the ratios of the CO(7-6) luminosity, L[CO(7-6)], to L(IR) are fairly tightly distributed (to within ~0.12 dex) and of little dependence on C(60/100). This makes L[CO(7-6)] a good SFR tracer, which is also less contaminated by active galactic nuclei than L(IR) and may also be much less sensitive to metallicity than CO(1-0). Furthermore, the logarithmic [NII]-to-CO(7-6) line ratios are fairly steeply (at a slope of -1.4) correlated with C(60/100), with a modest scatter (0.23 dex). This makes the ratio a useful estimator on C(60/100) with an implied uncertainty of ~0.17, accurate enough to separate a main-sequence disk star formation from a nuclear starburst for (U)LIRGs up to at least z ~ 3. With modern facilities such as ALMA and IRAM Plateau de Bure interferometers, our simple spectroscopic method will be able to not only measure the SF rates and SFR surface densities, but also probe the physical conditions of both ionized and warm/dense molecular gases in many high-z galaxies unveiled by WFIRST.
25. Roxana Lupu ( NASA Ames )
Co-authors: Mark Marley (NASA Ames); Michael Line (UCSC); Nikole Lewis (MIT); Caroline Morley (UCSC)Title: Characterization of giant exoplanet atmospheres with WFIRST-AFTA: confidence regions for methane abundance and cloud properties
Abstract: The coronagraph-equipped WFIRST-AFTA mission will be a powerful instrument for exoplanet characterization. The current design will be capable to directly image exoplanets down to a 10^-9 contrast level, and will include an integral field spectrograph covering the 0.60-0.97 micron range with a resolution of R~70. These specifications will enable the characterization of tens of gas- and ice- giants in the Solar neighborhood. In order to investigate the constraints on the atmospheric composition enabled by the WFIRST-AFTA instrument, we have assembled a spectral retrieval pipeline for extrasolar giant planet albedos, using a Monte Carlo Markov Chain ensemble sampler coupled with a two-cloud forward model for the planetary albedo. The retrieval technique was applied to simulated observations of Jupiter, Saturn, and Uranus around a sun-like star, as well as the HD99492c gas-giant. We consider a SNR range for the observations from 5 to 20 and consider the possibility of correlated noise over a 25 or 100 nanometer scale. In each case, we investigate the ability to constrain the methane abundance, the depths and single scattering albedos of the two cloud layers, as well as the optical depth and asymmetry factor for the top cloud. The surface gravity of the planet will be essentially unconstrained by these data alone. However, the gravity can be independently determined via the mass-radius relationship for imaged RV planets, and this constraint will tighten significantly the allowed range of methane abundance. In future work we will implement water and alkali opacities, and allow for a global scaling factor to account for radius uncertainties.
26. Clément Martinache ( Institut, d"Astrophysique Spatiale )
Co-authors: Dole; Guery; Montier; Nesvadba; Flores-Cacho; Altieri; Aghanim; Beelen; Bethermin; Chary; Douspis; Frye; Le Floc'h; Lagache; Pointecouteau; PugetTitle: Evidence for a z>2 cluster from NIR photometry of a Planck and Herschel candidate
Abstract: Clusters of galaxies studies are of particular importance in cosmology and astrophysics, especially at high redshift (z>2) where mass assembly is ongoing. We present the analysis of a z>2 cluster drawn from the sample of Planck and Herschel (Planck Collab., 2014, subm), characterized with large star formation rates (typically few 1000s Ms/yr). This particular target was followed-up by IRAC/Spitzer and HAWK-I/VLT in four near-infrared photometric bands. We show evidence of the presence of a z~2 galaxy cluster with high SFR, using color-color tracks, J-K and [3.6]-[4.5] color criteria. This exceptional structure could be a protocluster. Our program has 40 Spitzer targets of Planck and Herschel candidates, increasing the potential discoveries of z>2 clusters and paving the way for Euclid and WFIRST.
27. Daniel Charles Masters ( Infrared Processing and Analysis Center )
Co-authors: Peter Capak; Dan Stern; Jason Rhodes; Charles SteinhardtTitle: Mapping the Color-Redshift Relation of Galaxies: Towards Unbiased Photo-z Estimates for Weak Lensing Cosmology
Abstract: The growth of structure as measured by weak lensing has been identified as one of the most sensitive probes of dark energy and dark matter, and is one of the three key dark energy experiments proposed for WFIRST. However, the weak lensing measurement depends strongly on robust photometric redshifts, and is highly sensitive to systematic biases in these redshift estimates. We discuss our ongoing effort to develop an informed calibration of the color-redshift relation, in order to minimize the number of spectroscopic redshifts needed for photo-z calibration. This work will be applicable to both Euclid and WFIRST. Our approach involves developing an explicit mapping of the WFIRST N-dimensional color space using the machine learning technique known as the self-organizing map in conjunction with existing survey data. In addition to providing an optimal training set for machine learning, this method can be inverted to provide Bayesian priors for template fitting algorithms, which typically use either no prior, or ad hoc ones. Moreover, the color space mapping we are developing provides a means to automatically identify rare and interesting “Rosetta Stone” objects in the WFIRST data.
28. Jun Nishikawa ( NAOJ )
Co-authors: Naoshi Murakami; Masahito Oya; Kazuma Sato; Masaaki Horie; Takashi Kurokawa; Yosuke Tanaka; Motohide Tamura; Takayuki Kotani; Shiomi KumagaiTitle: Dark-hole control without modeling and enhanced extinction by pre-DM and pre-coronagraph
Abstract: We developed a dark-hole control algorithm without modeling. We stdied an enhancement of the dark-hole contrast by a pre-coronagraph with an upstream DM in addition to a contrast of a main coronagraph with a main DM. The pre-coronagraph should be low extinction (1/10 - 1/100) to produce an operatable wavefront at the main DM. We are developping a Lyot mask by super inc jet technology.
29. Bram Ochsendorf ( Leiden Observatory )
Co-authors: Tielens; A. G. G. M. Cox; N. L. J. Verdolini; S. Krijt; S. Salgado; F. Berné; O. Bernard; J. P. Kaper; L.Title: Radiation-pressure-driven dust waves inside bursting interstellar bubbles
Abstract: Massive stars drive the evolution of the interstellar medium through their radiative and mechanical energy input. After their birth, they form "bubbles" of hot gas surrounded by a dense shell. Traditionally, the formation of bubbles is explained through the input of a powerful stellar wind, even though direct evidence supporting this scenario is lacking. Analysis of Herschel-, WISE, and Spitzer- data has revealed that a vast multitude of interstellar bubbles show dust waves near the ionizing star, which demonstrates the importance of radiation pressure acting on an ionized gas flow through the bubble into the general interstellar medium. Dust waves provide a natural explanation for the long-standing problem on the presence of dust inside H II bubbles, offer a novel method to study dust in H II regions, and provide direct evidence that bubbles are relieving their pressure into the interstellar medium through a champagne flow, acting as a probe of the radiative interaction of a massive star with its surroundings. We have examined the implications of our study for the environments of super star clusters formed in ultraluminous infrared galaxies, merging galaxies, and the early Universe, which occur in very luminous and dense environments and where radiation pressure is expected to dominate the dynamical evolution.
30. Nor Pirzkal ( STScI )
Co-authors: Sangeeta Malhotra; James Rhoads; FIGS TeamTitle: The Faint Infrared Survey: FIGS
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Abstract: We describe and present early results from a new, deep Hubble Space Telescope in infrared survey. This unique project uses the WFC3 IR grism G102,to produce low resolution spectra for 6000 sources in 4 separate fields. FIGS will:(1) Probe the reionization epoch by spectroscopy of galaxies at z = 5.5-8.5, whether or not they show Lyman-alpha (LyA) line emission. Continuum breaks are hard to detect from the ground and LyA lines may be scarce at these redshifts. Spectroscopic redshifts will probe galaxy clustering and improve luminosity measurements, thereby improving estimates of reionizing photons by at least 40%.(2) Robustly measure the fraction of galaxies with high EW LyA, to measure the neutral fraction of the IGM. We are sensitive to LyA lines in the central period of reionization where we expect to see a change in LyA fraction.(3) Illuminate the formation processes of early type galaxies at 1<z<2, down to a few 10^9 solar masses.(4) Study star-formation, dust extinction and metallicity evolution during the peak of star-formation at z=1-2, using hundreds of low-mass emission line galaxies.
31. Jeonghyun Pyo ( Korea Astronomy and Space Science Institute (KASI) )
Co-authors: Il-Joong Kim (KASI); Woong-Seob Jeong (KASI; UST); Dae-Hee Lee (KASI); Bongkon Moon (KASI); Youngsik Park (KASI); Sung-Joon Park (KASI); Won-Kee Park (KASI); Duk-Hang Lee (UST; KASI); Uk-Won Nam (KASI); Wonyong Han (KASI; UST); Kwang-Il Seon (KASI; UST); Toshio Matsumoto (ASIAA; ISAS/JAXA); Min Gyu Kim (SNU); Hyung Mok Lee (SNU); Hong-Young Park (SaTReC); Chol Lee (SaTReC); Seung-Wu Rhee (KARI);Title: Near-Infrared Wide Area Surveys with Small Space Telescope, MIRIS
Abstract: MIRIS (Multi-purpose Infrared Imaging System) is the main payload of Korean STSAT-3 (Science and Technology Satellite 3) launched in late November 2013. After three months of verification phase, the main phases for science missions started from March 2014 and will continue for a year and a month. The major science missions of MIRIS are i) the observations of various fields with I- and H-bands for the study of infrared background and ii) the Paα-line survey observations along the Galactic plane for the comparative study of the warm ionized medium. For last 9 months, we finished the I- and H-bands observations of 10° × 10° areas centered at the north ecliptic and north and south galactic poles, and covered the Galactic plane from the longitude of 285° to 100° with the Paα survey. Several targets of interest, such as Large and Small Magellanic Clouds, were also observed. MIRIS is now in the 4th main phase to cover the remaining half of the Galactic plane, after which the user time is open to public. This contribution introduces the science missions of MIRIS with the preliminary results from observations so far.
32. Swara Ravindranath ( Space Telescope Science Institute )
Co-authors: Van Dixon; Chris Willott; and the NIRISS Science TeamTitle: Wide-Field Slitless Spectroscopy with NIRISS on JWST
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Abstract: In this talk, I will provide an overview of the Near-Infrared Imaging and Slitless Spectrograph (NIRISS) instrument on the James Webb Space Telescope (JWST), and its capabilities for wide-field slitless spectroscopy (WFSS). In the WFSS mode, NIRISS renders a spectrum for every object in the field of view with a resolving power, R=150 over the wavelength range 0.8 - 2.25 microns. Two identical grisms oriented with orthogonal dispersion directions are used in NIRISS to alleviate the problems with overlap of spectra in crowded fields. The NIRISS WFSS mode is designed to enable the detection of Lyman-alpha emission lines, and the Lyman-break feature in the spectra of high redshift (z=6-17) galaxies, to probe the first ionizing sources in the early Universe. Every WFSS observation will also contain a wealth of information on the foreground objects, creating a unique resource of optical emission line spectra for the faintest galaxies at lower redshifts. The deep spectroscopic surveys using NIRISS on JWST is expected to offer interesting complementarity with the large area WFIRST surveys.
33. Nicholas P. Ross ( Drexel/Edinburgh Universities )
Co-authors: John Timlin (Drexel); Gordon Richards (Drexel); Mark Lacy (NRAO); and the SpIES TeamTitle: First Science Results from the SpIES
Abstract: The Spitzer-IRAC Equatorial Survey, SpIES, is a Exploration Science program using Warm Spitzer to map over 100deg^2 of the Equatorial SDSS Stripe 82 field, and is the largest extragalactic area surveyed by Spitzer. The primary science drivers are: the measurement of z>3 quasar clustering and luminosity function in order to test different ``AGN feedback'' models; to identify obscured AGN (and take advantage of the wide range of multi-wavelength, multi-epoch ancillary data on the Stripe 82 field); identify z>6 quasars, and support other wide-field ancillary science. With our observations very recently completed, we present the first preliminary science results from SpIES and see how this survey will impact future space-based infrared surveys such as JWST and WFIRST-AFTA.
34. Daniel Stern ( JPL )
Title: Surprising New Insights into Quasars from the WISE Satellite
Abstract: In most quasars, obscuring material along the line of sight shields us from directly viewing the inner regions around the central,accreting supermassive black hole. This obscuring material is heated, and emits strongly in the mid-infrared. The Wide-field Infrared Survey Explorer, or WISE, has recently mapped the entire sky in mid-infrared light with exquisite depth and clarity. WISE has allowed us to find luminous quasars across the whole sky due to this heated material, more than tripling the number of quasars known. I will discuss several surprising new insights into quasars that have come out of this work. In brief, the dominant paradigms do not match our observations, with potentially important implications for the role of quasars in the growth of galaxies. I will discuss how this work will be enabled by the deeper data currently being obtained by the NEOWISE (nee WISE) mission. I will conclude by discussing how these studies both impact and will be further enabled by the Euclid and WFIRST satellites. In particular, flagging WISE-identified AGN may be essential for achieving the challenging photometric redshift requirements of both Euclid and WFIRST.
35. Hiroyuki Tetsu ( Tokyo Institute of Technology )
Co-authors: T.; Nakamoto (Tokyo Institute of Technology)Title: Gravitational Contraction and Fragmentation of Filamentary Molecular Clouds
Abstract: Herschel Space Observatory reveals the ubiquitous existence of filamentary structures in molecular clouds as star-formation site (Andre’ et al. 2010). Additionally, quite recently, it is suggested from observations that thermally super-critical filaments may undergo gravitational contraction (Arzoumanian et al. 2013). On the other hand, according to scenarios that describe star-formation through contraction and fragmentation of filamentary molecular clouds, the switch of main heating process from external heating to internal compressional heating determines the Jeans mass of fragments (Inutsuka and Miyama 1992, 1997, Masunaga & Inutsuka 1999). However, there are some important problems in transient phase from radial contraction to axial fragmentation. How does the temperature, which is determined by radiative transfer, restrict the radial deceleration? And consequently, when the fragmentations appear and how massive they are? To study these problems, we perform two-dimensional radiation hydrodynamics calculations with self-gravity using ZEUS-2D (Stone and Norman 1992) and Flux Limited Diffusion approximation algorithm (Turner and Stone 2001) with some modifications on the basis of Douglas-Rachford operator splitting scheme (Douglas-Rachford 1956). To quantify when two-dimensionality appears, the Fourier analysis of axial perturbations is performed. As a result, we obtain the threshold as the central density of filaments. Interestingly, there is a considerable difference between density at which isothermality breaks down and two-dimensionality appears. The fragment mass estimated from the density with which the two-dimensionality appears could be extremely low, ~3 Jupiter mass in a typical case, being comparable with semi-brown dwarfs or free-floating planets. In this poster, we focus on how these processes might be observed.
36. Karun G Thanjavur ( University of Victoria (UVic) )
Co-authors: Karun Thanjavur; Justin Albert; Chris Pritchet; Divya Bhatnagar; Paul Kovacs (University of Victoria); Yorke Brown (Dartmouth College); Christopher Stubbs (Harvard University); Susana Deustua (STSci); Claire Cramer (NIST); Keith Vanderlinde (University of Toronto); Matt Dobbs (McGill University); Arnold Gaertner (National Research Council of Canada)Title: ALTAIR: Precision Spectro-Photometric Calibration via Artificial Light Sources above the Atmosphere
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Abstract: In the era of precision cosmology, continued progress toward our understanding of the Universe, e.g., the properties of Dark Energy via SNeIa luminosity distances measured by ongoing/ upcoming large, panchromatic surveys, requires unprecedented spectro-photometric precision (better than 1%) in absolute flux measurement. At present, even though laboratory and solar photometry/radiometry routinely achieve precision on the order of few parts in ten thousand, photometric calibration in astronomy has plateaued at the level of a few percent despite sustained efforts. In this context, we present an overview of our project, ALTAIR, aimed at improving the calibration precision by using a high altitude (20Km and higher) balloon-borne laser light source as the primary spectro-photometric calibrator. We present current results from the twelve successful flights to date, as well as comparisons with stellar and lunar observations. Our timeline is to perfect the technique for surveys such as the ongoing Pan-STARRS, and LSST beginning later this decade. The ALTAIR platform is equally applicable to infrared and other observing wavebands, and is critical to tying together space missions such as WFIRST with the large ground-based surveys. In addition, observations of gravitational waves in the polarized CMB require similar polarimetric and radiometric precision, and we briefly present our progress on calibrated microwave sources above the atmosphere as well.
37. Rodger I Thompson ( Steward Observatory, University of Arizona )
Co-authors: Xiaohui Fan; Brant RobertsonTitle: Wide Deep Imaging with an AFTA Dichroic Imager
Abstract: Use of the 2.4m aperture afforded by AFTA and a dichroic imager that views the same field of view in 4 different filters provides greatly enhanced scientific opportunities. One of these opportunities is the creation of four separate one square degree fields imaged to fainter than 31AB mag. 5 sigma in eight spectral bands per 0.11 arc second pixel. These fields provide legacy data to the community for extragalactic studies of unparalleled spatial extent and sensitivity. These fields compliment the much smaller spatial scale high resolution imaging of JWST and greatly surpass all of the HST deep fields in both sensitivity and spatial scale. They are made possible by a unique dichroic imager that accomplishes all of the WFIRST science program in one year of observations, spends one year imaging the fields and allocates the remaining years to General Observer Science. Details of the fields, the enabled science and the imager concept are discussed in the presentation.
38. Vladimir Tichy ( Czech Technical University in Prague )
Co-authors: David N. Burrows; Rene Hudec; Zachary PrieskornTitle: Optical Study of Nano-Satellite X-Ray Monitor
Abstract: The Schmidt lobster eye design for a grazing incidence X-ray optics provides wide field of view of the order of many degrees, for this reason it can be a convenient approach for the construction of space X-ray monitors. Schmidt lobster eye is possible to assemble in various scales of dimensions and also dimensions and focal lengths acceptable for nano-class satellites are possible. Draft of nano-class space mission providing monitoring of specific sky area is presented. Preliminary optical design study for such mission is performed. Two of possible opticle designs are presented. For those designs, field of view, effective input area and other basic optical parameters are calculated.
39. Chao-Wei Tsai ( JPL )
Co-authors: Peter Eisenhardt; Daniel Stern; Jingwen Wu; Roberto AssefTitle: Discovery of the Most Luminous Galaxies in the Universe with WISE
Abstract: Wide area surveys enable unusual objects to be found. I present a class of distant dust-enshrouded galaxies with extremely high luminosity, including several “Extremely Luminous Infrared Galaxies” that reach 10^14 L_Sun. Selected by their extreme red colors in WISE bands, their SEDs incorporating WISE, Spitzer, and Herschel photometry indicate hot dust dominates the bolometric luminosity. These sources are likely powered by highly obscured active galactic nuclei (AGN), are unlikely to be lensed, and may be as common or more common than unobscured quasars of this luminosity. The existence of ELIRGs at z > 3 constrains the supermassive black hole (SMBH) growth history, suggesting that these SMBH's are born with large mass, or have a very rapid mass assembly, presumably by chaotic accretion. They are different from normal populations in their M-sigma relation and FIR-radio correlation. Their low source density (~ 10^-5 of LIRGs' at similar redshift) implies that these objects are intrinsically rare, or are a short-lived phase in a more numerous population. If the latter is the case, these hot, dust-enshrouded galaxies may be in an early stage in the interplay between AGN and galaxies.
40. Kenichi Yano ( University of Tokyo, ISAS/JAXA )
Co-authors: T. Nakagawa; N. Isobe; M. ShirahataTitle: Ionizing Photon Deficit in Ultraluminous Infrared Galaxies Probed with AKARI
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Abstract: We carried out systematic observations of the H I Br-alpha line (4.05 micron) in 51 nearby (z<0.3) ultraluminous infrared galaxies (ULIRGs) to quantitatively estimate star formation rates (SFRs) with AKARI. The Br-alpha line is predicted to be the brightest among the H I recombination lines in ULIRGs under the high dust-extinction condition (visual extinction Av>15 mag) and thus is the most suitable for probing star formation in ULIRGs. We find that SFRs derived from the Br-alpha line luminosity are on average only one third of those needed to explain the total infrared luminosity even in ULIRGs optically classified as H II galaxies, which are thought to be 100% energized by starburst. We attribute this to the absorption of ionizing photons by dust within H II regions. Our result indicates that other lines tracing ionizing photons (e.g. other H I recombination lines) also show a deficit in a population of infrared-luminous, dust-rich galaxies. The WFIRST/AFTA grism will provide wide-field slitless spectroscopy which covers H I Paschen and Balmer lines in galaxies with redshift of 0<z<0.5 and 1<z<2, respectively. Although careful consideration of dust extinction is required for these lines, WFIRST will enable us to investigate this problem in a very large number of galaxies.
41. Wei Zhu ( Ohio State University )
Co-authors: A. Gould; J. Yee; et al.Title: Spitzer as Microlens Parallax Satellite: Mass and Distance Measurement for Binary System OGLE-2014-BLG-1050L
Abstract: We report the first mass and distance measurement of a caustic-crossing binary system OGLE-2014-BLG-1050L using the space-based microlense parallax method. Spitzer captured the second caustic-crossing of the event, which happened ∼10 days before that seen from ground. Due to the coincidence that the source-lens relative motion was almost parallel to the direction of binary-lens axis, the four-fold degeneracy which was known before only to happen in single-lens events appears in this case, leading to either a lower-mass (0.2 M_⊙ plus 0.1 M_⊙) binary at ∼1.3 kpc or a higher-mass (0.8 M_⊙ plus 0.4 M_⊙) binary at ∼3.5 kpc. However, the later solution is preferred by several considerations, including blending and lensing probability and Δ χ^2=10. OGLE-2014-BLG-1050L presents the power of microlens parallax in probing the galactic distribution of stellar binaries.
42. Andrew Battisti ( UMass Amherst )
Co-authors: D. Calzetti; R.-R. Chary; B. D. Johnson; & D. ElbazTitle: Continuous Mid-IR SFR Indicators & Characterizing Dust Attenuation
Abstract: We calibrate continuous, monochromatic star formation rate (SFR) indicators over the mid-infrared wavelength range of 6-70 microns. We use a sample of 58 star forming galaxies (SFGs) in the Spitzer-SDSS-GALEX Spectroscopic Survey (SSGSS) at z<0.2, for which there is a rich suite of multi-wavelength photometry and spectroscopy from the ultraviolet through to the infrared. We find that our continuous SFR indicators are consistent with recent monochromatic calibrations in the local universe. In the era of the James Webb Space Telescope (JWST) this will become a flexible tool to be applied to any galaxy up to z=3.
In addition, we present preliminary results to calibrate the dust attenuation for a large sample of SFGs as a function of their physical properties. Following the method of Calzetti et al. (1994), the dust attenuation is characterized through the UV power-law index and the Balmer optical depth. Using this approach we aim to create a general dust attenuation curve for SFGs which will span a large range of galaxy parameters. We will utilize the wealth of multi-wavelength data available from GALEX, SDSS, Spitzer, and Herschel to gain insight into how various galaxy properties correlate with dust attenuation in order to ensure that appropriate corrections can be made in future surveys. This study will set the groundwork for extensions in the future to cover a wide range of redshift to improve the ability of future cosmological studies, specifically the Euclid mission.
