78 research outputs found
Bostonia: v. 64, no. 1
Founded in 1900, Bostonia magazine is Boston University's main alumni publication, which covers alumni and student life, as well as university activities, events, and programs
Interpretation of the ARCADE 2 Absolute Sky Brightness Measurement
We use absolutely calibrated data between 3 and 90 GHz from the 2006 balloon flight of the ARCADE 2 instrument, along with previous measurements at other frequencies, to constrain models of extragalactic emission. Such emission is a combination of the cosmic microwave background (CMB) monopole, Galactic foreground emission, the integrated contribution of radio emission from external galaxies, any spectral distortions present in the CMB, and any other extragalactic source. After removal of estimates of foreground emission from our own Galaxy, and an estimated contribution of external galaxies, we present fits to a combination of the flat-spectrum CMB and potential spectral distortions in the CMB.We find 2σ upper limits to CMB spectral distortions ofμ \u3c 6×10−4 and |Yff| \u3c 1×10−4. We also find a significant detection of a residual signal beyond that, which can be explained by the CMB plus the integrated radio emission from galaxies estimated from existing surveys. This residual signal may be due to an underestimated galactic foreground contribution, an unaccounted for contribution of a background of radio sources, or some combination of both. The residual signal is consistent with emission in the form of a power law with amplitude 18.4 ± 2.1 K at 0.31 GHz and a spectral index of −2.57 ± 0.05
ARCADE 2 Observations of Galactic Radio Emission
We use absolutely calibrated data from the ARCADE 2 flight in 2006 July to model Galactic emission at frequencies 3, 8, and 10 GHz. The spatial structure in the data is consistent with a superposition of free–free and synchrotron emission. Emission with spatial morphology traced by the Haslam 408 MHz survey has spectral index βsynch = −2.5±0.1, with free–free emission contributing 0.10±0.01 of the total Galactic plane emission in the lowest ARCADE 2 band at 3.15 GHz. We estimate the total Galactic emission toward the polar caps using either a simple plane-parallel model with csc |b| dependence or a model of high-latitude radio emission traced by the COBE/FIRAS map of C ii emission. Both methods are consistent with a single power law over the frequency range 22 MHz to 10 GHz, with total Galactic emission toward the north polar cap TGal = 10.12 ± 0.90 K and spectral index β = −2.55 ± 0.03 at reference frequency 0.31 GHz. Emission associated with the plane-parallel structure accounts for only 30% of the observed high-latitude sky temperature, with the residual in either a Galactic halo or an isotropic extragalactic background. The well-calibrated ARCADE 2 maps provide a new test for spinning dust emission, based on the integrated intensity of emission from the Galactic plane instead of cross-correlations with the thermal dust spatial morphology. The Galactic plane intensity measured by ARCADE 2 is fainter than predicted by models without spinning dust and is consistent with spinning dust contributing 0.4 ± 0.1 of the Galactic plane emission at 23 GHz
Persistent starspot signals on M dwarfs: multi-wavelength Doppler observations with the Habitable-zone Planet Finder and Keck/HIRES
Young, rapidly-rotating M dwarfs exhibit prominent starspots, which create
quasiperiodic signals in their photometric and Doppler spectroscopic
measurements. The periodic Doppler signals can mimic radial velocity (RV)
changes expected from orbiting exoplanets. Exoplanets can be distinguished from
activity-induced false positives by the chromaticity and long-term incoherence
of starspot signals, but these qualities are poorly constrained for
fully-convective M stars. Coherent photometric starspot signals on M dwarfs may
persist for hundreds of rotations, and the wavelength dependence of starspot RV
signals may not be consistent between stars due to differences in their
magnetic fields and active regions. We obtained precise multi-wavelength RVs of
four rapidly-rotating M dwarfs (AD Leo, G 227-22, GJ 1245B, GJ 3959) using the
near-infrared (NIR) Habitable-zone Planet Finder, and the optical Keck/HIRES
spectrometer. Our RVs are complemented by photometry from Kepler, TESS, and the
Las Cumbres Observatory (LCO) network of telescopes. We found that all four
stars exhibit large spot-induced Doppler signals at their rotation periods, and
investigated the longevity and optical-to-NIR chromaticity for these signals.
The phase curves remain coherent much longer than is typical for Sunlike stars.
Their chromaticity varies, and one star (GJ 3959) exhibits optical and NIR RV
modulation consistent in both phase and amplitude. In general, though, we find
that the NIR amplitudes are lower than their optical counterparts. We conclude
that starspot modulation for rapidly-rotating M stars frequently remains
coherent for hundreds of stellar rotations, and gives rise to Doppler signals
that, due to this coherence, may be mistaken for exoplanets.Comment: Accepted for publication in the Astrophysical Journa
Scaling K2. VI. Reduced Small Planet Occurrence in High Galactic Amplitude Stars
In this study, we performed a homogeneous analysis of the planets around FGK
dwarf stars observed by the Kepler and K2 missions, providing spectroscopic
parameters for 310 K2 targets -- including 239 Scaling K2 hosts -- observed
with Keck/HIRES. For orbital periods less than 40 days, we found that the
distribution of planets as a function of orbital period, stellar effective
temperature, and metallicity was consistent between K2 and Kepler, reflecting
consistent planet formation efficiency across numerous ~1 kpc sight-lines in
the local Milky Way. Additionally, we detected a 3X excess of sub-Saturns
relative to warm Jupiters beyond 10 days, suggesting a closer association
between sub-Saturn and sub-Neptune formation than between sub-Saturn and Jovian
formation. Performing a joint analysis of Kepler and K2 demographics, we
observed diminishing super-Earth, sub-Neptune, and sub-Saturn populations at
higher stellar effective temperatures, implying an inverse relationship between
formation and disk mass. In contrast, no apparent host-star spectral-type
dependence was identified for our population of Jupiters, which indicates
gas-giant formation saturates within the FGK mass regimes. We present support
for stellar metallicity trends reported by previous Kepler analyses. Using GAIA
DR3 proper motion and RV measurements, we discovered a galactic location trend:
stars that make large vertical excursions from the plane of the Milky Way host
fewer super-Earths and sub-Neptunes. While oscillation amplitude is associated
with metallicity, metallicity alone cannot explain the observed trend,
demonstrating that galactic influences are imprinted on the planet population.
Overall, our results provide new insights into the distribution of planets
around FGK dwarf stars and the factors that influence their formation and
evolution.Comment: 28 Pages, 12 Figures, 3 Tables; Accepted for Publication A
TOI-561 b: A Low Density Ultra-Short Period "Rocky" Planet around a Metal-Poor Star
TOI-561 is a galactic thick disk star hosting an ultra-short period (0.45 day
orbit) planet with a radius of 1.37 R, making it one of the most
metal-poor ([Fe/H] = -0.41) and oldest (10 Gyr) sites where an
Earth-sized planet has been found. We present new simultaneous radial velocity
measurements (RVs) from Gemini-N/MAROON-X and Keck/HIRES, which we combined
with literature RVs to derive a mass of M=2.24 0.20 M.
We also used two new Sectors of TESS photometry to improve the radius
determination, finding R=, and confirming that
TOI-561 b is one of the lowest-density super-Earths measured to date (=
4.8 0.5 g/cm). This density is consistent with an iron-poor rocky
composition reflective of the host star's iron and rock-building element
abundances; however, it is also consistent with a low-density planet with a
volatile envelope. The equilibrium temperature of the planet (2300 K)
suggests that this envelope would likely be composed of high mean molecular
weight species, such as water vapor, carbon dioxide, or silicate vapor, and is
likely not primordial. We also demonstrate that the composition determination
is sensitive to the choice of stellar parameters, and that further measurements
are needed to determine if TOI-561 b is a bare rocky planet, a rocky planet
with an optically thin atmosphere, or a rare example of a non-primordial
envelope on a planet with a radius smaller than 1.5 R.Comment: Accepted to AJ on 11/28/202
TOI-1670 c, a 40-day Orbital Period Warm Jupiter in a Compact System, is Well-aligned
We report the measurement of the sky-projected obliquity angle of
the Warm Jovian exoplanet TOI-1670 c via the Rossiter-McLaughlin effect as part
of the Stellar Obliquities in Long-period Exoplanet Systems (SOLES) project. We
observed the transit window during UT 20 April 2023 for 7 continuous hours with
NEID on the 3.5 m WIYN Telescope at Kitt Peak National Observatory. TOI-1670
hosts a sub-Neptune (P ~11 days; planet b) interior to the Warm Jovian (P ~40
days; planet c), which presents an opportunity to investigate the dynamics of a
Warm Jupiter with an inner companion. Additionally, TOI-1670 c is now among the
longest-period planets to date to have its sky-projected obliquity angle
measured. We find planet c is well-aligned to the host star, with =
-0.3 +/- 2.2 degrees. TOI-1670 c joins a growing census of aligned Warm
Jupiters around single stars and aligned planets in multi-planet systems.Comment: 11 pages, 2 figures, 1 table. Accepted to ApJ Letter
Persistent Starspot Signals on M Dwarfs: Multiwavelength Doppler Observations with the Habitable-zone Planet Finder and Keck/HIRES
Young, rapidly rotating M dwarfs exhibit prominent starspots, which create quasiperiodic signals in their photometric and Doppler spectroscopic measurements. The periodic Doppler signals can mimic radial velocity (RV) changes expected from orbiting exoplanets. Exoplanets can be distinguished from activity-induced false positives by the chromaticity and long-term incoherence of starspot signals, but these qualities are poorly constrained for fully convective M stars. Coherent photometric starspot signals on M dwarfs may persist for hundreds of rotations, and the wavelength dependence of starspot RV signals may not be consistent between stars due to differences in their magnetic fields and active regions. We obtained precise multiwavelength RVs of four rapidly rotating M dwarfs (AD Leo, G227-22, GJ 1245B, GJ 3959) using the near-infrared (NIR) Habitable-zone Planet Finder and the optical Keck/HIRES spectrometer. Our RVs are complemented by photometry from Kepler, TESS, and the Las Cumbres Observatory network of telescopes. We found that all four stars exhibit large spot-induced Doppler signals at their rotation periods, and investigated the longevity and optical-to-NIR chromaticity for these signals. The phase curves remain coherent much longer than is typical for Sunlike stars. Their chromaticity varies, and one star (GJ 3959) exhibits optical and NIR RV modulation consistent in both phase and amplitude. In general, though, we find that the NIR amplitudes are lower than their optical counterparts. We conclude that starspot modulation for rapidly rotating M stars frequently remains coherent for hundreds of stellar rotations and gives rise to Doppler signals that, due to this coherence, may be mistaken for exoplanets
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