29 research outputs found
Empirical Constraints on the First Stars and Quasars
Empirical studies of the first generation of stars and quasars in the
Universe will likely become feasible over the next decade. The Next Generation
Space Telescope will provide direct imaging and photometry of sub-galactic
objects at redshifts above z=10, while microwave anisotropy experiments, such
as MAP or Planck, will set constraints on the ionization history of the
intergalactic medium due to these sources. We describe the expected signals
that will be detectable with these future instruments.Comment: 14 pages, invited contribution to Proc. of 9th Annual October
Astrophysics Conference in Maryland, "After the Dark Ages: When Galaxies Were
Young (the Universe at 2 < z < 5", College Park, October 199
The correlation between the distribution of galaxies and 21cm emission at high redshifts
Deep surveys have recently discovered galaxies at the tail end of the epoch
of reionization. In the near future, these discoveries will be complemented by
a new generation of low-frequency radio observatories that will map the
distribution of neutral hydrogen in the intergalactic medium through its
redshifted 21cm emission. In this paper we calculate the expected
cross-correlation between the distribution of galaxies and intergalactic 21cm
emission at high redshifts. We demonstrate using a simple model that overdense
regions are expected to be ionized early as a result of their biased galaxy
formation. This early phase leads to an anti-correlation between the 21cm
emission and the overdensities in galaxies, matter, and neutral hydrogen.
Existing Ly-alpha surveys probe galaxies that are highly clustered in overdense
regions. By comparing 21cm emission from regions near observed galaxies to
those away from observed galaxies, future observations will be able to test
this generic prediction and calibrate the ionizing luminosity of high-redshift
galaxies.Comment: 10 pages, 6 figures. Submitted to MNRA
Detection Of KOI-13.01 Using The Photometric Orbit
We use the KOI-13 transiting star-planet system as a test case for the
recently developed BEER algorithm (Faigler & Mazeh 2011), aimed at identifying
non-transiting low-mass companions by detecting the photometric variability
induced by the companion along its orbit. Such photometric variability is
generated by three mechanisms, including the beaming effect, tidal ellipsoidal
distortion, and reflection/heating. We use data from three Kepler quarters,
from the first year of the mission, while ignoring measurements within the
transit and occultation, and show that the planet's ephemeris is clearly
detected. We fit for the amplitude of each of the three effects and use the
beaming effect amplitude to estimate the planet's minimum mass, which results
in M_p sin i = 9.2 +/- 1.1 M_J (assuming the host star parameters derived by
Szabo et al. 2011). Our results show that non-transiting star-planet systems
similar to KOI-13.01 can be detected in Kepler data, including a measurement of
the orbital ephemeris and the planet's minimum mass. Moreover, we derive a
realistic estimate of the amplitudes uncertainties, and use it to show that
data obtained during the entire lifetime of the Kepler mission, of 3.5 years,
will allow detecting non-transiting close-in low-mass companions orbiting
bright stars, down to the few Jupiter mass level. Data from the Kepler Extended
Mission, if funded by NASA, will further improve the detection capabilities.Comment: Accepted to AJ on October 4, 2011. Kepler Q5 Long Cadence data will
become publicly available on MAST by October 23. Comments welcome (V2: minor
changes, to reflect proof corrections
A New Era in Extragalactic Background Light Measurements: The Cosmic History of Accretion, Nucleosynthesis and Reionization
(Brief Summary) What is the total radiative content of the Universe since the
epoch of recombination? The extragalactic background light (EBL) spectrum
captures the redshifted energy released from the first stellar objects,
protogalaxies, and galaxies throughout cosmic history. Yet, we have not
determined the brightness of the extragalactic sky from UV/optical to
far-infrared wavelengths with sufficient accuracy to establish the radiative
content of the Universe to better than an order of magnitude. Among many
science topics, an accurate measurement of the EBL spectrum from optical to
far-IR wavelengths, will address: What is the total energy released by stellar
nucleosynthesis over cosmic history? Was significant energy released by
non-stellar processes? Is there a diffuse component to the EBL anywhere from
optical to sub-millimeter? When did first stars appear and how luminous was the
reionization epoch? Absolute optical to mid-IR EBL spectrum to an
astrophysically interesting accuracy can be established by wide field imagingat
a distance of 5 AU or above the ecliptic plane where the zodiacal foreground is
reduced by more than two orders of magnitude.Comment: 7 pages; Science White Paper for the US Astro 2010-2020 Decadal
Survey. If interested in further community-wide efforts on this topic please
contact the first autho
The Dynamic X-ray Sky of the Local Universe
Over the next decade, we can expect time domain astronomy to flourish at
optical and radio wavelengths. In parallel with these efforts, a dedicated
transient "machine" operating at higher energies (X-ray band through soft
gamma-rays) is required to reveal the unique subset of events with variable
emission predominantly visible above 100 eV. Here we focus on the transient
phase space never yet sampled due to the lack of a sensitive, wide-field and
triggering facility dedicated exclusively to catching high energy transients
and enabling rapid coordinated multi-wavelength follow-up. We first describe
the advancements in our understanding of known X-ray transients that can only
be enabled through such a facility and then focus on the classes of transients
theoretically predicted to be out of reach of current detection capabilities.
Finally there is the exciting opportunity of revealing new classes of X-ray
transients and unveiling their nature through coordinated follow-up
observations at longer wavelengths.Comment: 8 pages, 2 figures; White Paper submitted to the Astro2010 SSE pane