As described in sect; 2.3, each HSsub 4 unit is controlled by a single control computer running Linux with a special kernel that is capable of real-time operations. In addition, a node-computer is ...responsible for weather sensing and synchronizing the time to the GPS time. A large suite of software is running on the control and node computers, responsible for the instrument control. We broadly classify the control software components to "low-level", meaning direct control of instruments, and "high-level", referring to more general observatory control, usually connected to the "low-level" software. The control of the telescope mount is performed through a Xenomai-based (real-time) character device driver, called the scope module. This module depends on the basic built-in printer port control modules of Linux. When the scope kernel module is loaded, a number of initial parameters are supplied, such as the choice of the hemisphere (to determine the direction of tracking), the resolution of the axes, settings for ramping up the motors to maximal slewing speed, and the level of verbosity.
We report the discovery of HAT-P-24b, a transiting extrasolar planet orbiting the moderately bright V = 11.818 F8 dwarf star GSC 0774--01441, with a period P = 3.3552464 ? 0.0000071 days, transit ...epoch Tc = 2455216.97669 ? 0.00024 (BJD)11, and transit duration 3.653 ? 0.025 hr. The host star has a mass of 1.191 ? 0.042 M , radius of 1.317 ? 0.068 R , effective temperature 6373 ? 80 K, and a low metallicity of Fe/H = -0.16 ? 0.08. The planetary companion has a mass of 0.681 ? 0.031 M J and radius of 1.243 ? 0.072 R J yielding a mean density of 0.439 ? 0.069 g cm-3. By repeating our global fits with different parameter sets, we have performed a critical investigation of the fitting techniques used for previous Hungarian-made Automated Telescope planetary discoveries. We find that the system properties are robust against the choice of priors. The effects of fixed versus fitted limb darkening are also examined. HAT-P-24b probably maintains a small eccentricity of e = 0.052+0.022 --0.017, which is accepted over the circular orbit model with false alarm probability 5.8%. In the absence of eccentricity pumping, this result suggests that HAT-P-24b experiences less tidal dissipation than Jupiter. Due to relatively rapid stellar rotation, we estimate that HAT-P-24b should exhibit one of the largest known Rossiter-McLaughlin effect amplitudes for an exoplanet ( Delta *DV RM 95 m s--1) and thus a precise measurement of the sky-projected spin-orbit alignment should be possible.
We present the discovery of two transiting exoplanets. HAT-P-28b orbits a V = 13.03 G3 dwarf star with a period P = 3.2572 days and has a mass of 0.63 ? 0.04 M J and a radius of 1.21+0.11 -- 0.08 R J ...yielding a mean density of 0.44 ? 0.09 g cm--3. HAT-P-29b orbits a V = 11.90 F8 dwarf star with a period P = 5.7232 days and has a mass of 0.78+0.08 -- 0.04 M J and a radius of 1.11+0.14 -- 0.08 R J yielding a mean density of 0.71 ? 0.18 g cm--3. We discuss the properties of these planets in the context of other known transiting planets.
We report the discovery of two new transiting extrasolar planets. HAT-P-18b orbits the V = 12.759 K2 dwarf star GSC 2594--00646, with a period P = 5.508023 ? 0.000006 days, transit epoch Tc = ...2454715.02174 ? 0.00020 (BJD), and transit duration 0.1131 ? 0.0009 days. The host star has a mass of 0.77 ? 0.03 M , radius of 0.75 ? 0.04 R , effective temperature 4803 ? 80 K, and metallicity Fe/H = +0.10 ? 0.08. The planetary companion has a mass of 0.197 ? 0.013 M J and radius of 0.995 ? 0.052 R J, yielding a mean density of 0.25 ? 0.04 g cm--3. HAT-P-19b orbits the V = 12.901 K1 dwarf star GSC 2283--00589, with a period P = 4.008778 ? 0.000006 days, transit epoch Tc = 2455091.53417 ? 0.00034 (BJD), and transit duration 0.1182 ? 0.0014 days. The host star has a mass of 0.84 ? 0.04 M , radius of 0.82 ? 0.05 R , effective temperature 4990 ? 130 K, and metallicity Fe/H = +0.23 ? 0.08. The planetary companion has a mass of 0.292 ? 0.018 M J and radius of 1.132 ? 0.072 R J, yielding a mean density of 0.25 ? 0.04 g cm--3. The radial velocity residuals for HAT-P-19 exhibit a linear trend in time, which indicates the presence of a third body in the system. Comparing these observations with theoretical models, we find that HAT-P-18b and HAT-P-19b are each consistent with a hydrogen-helium-dominated gas giant planet with negligible core mass. HAT-P-18b and HAT-P-19b join HAT-P-12b and WASP-21b in an emerging group of low-density Saturn-mass planets, with negligible inferred core masses. However, unlike HAT-P-12b and WASP-21b, both HAT-P-18b and HAT-P-19b orbit stars with super-solar metallicity. This calls into question the heretofore suggestive correlation between the inferred core mass and host star metallicity for Saturn-mass planets.
Abstract
We report the discovery of four transiting giant planets around K dwarfs. The planets HATS-47b, HATS-48Ab, HATS-49b, and HATS-72b have masses of
,
,
, and
, respectively, and radii of
,
,
, ...and
, respectively. The planets orbit close to their host stars with orbital periods of
days,
days,
days, and
days, respectively. The hosts are main-sequence K dwarfs with masses of
,
,
, and
, and with
V
-band magnitudes of
,
,
and
. The super-Neptune HATS-72b (a.k.a. WASP-191b and TOI 294.01) was independently identified as a transiting planet candidate by the HATSouth, WASP, and
TESS
surveys, and we present a combined analysis of all of the data gathered by each of these projects (and their follow-up programs). An exceptionally precise mass is measured for HATS-72b thanks to high-precision radial velocity (RV) measurements obtained with VLT/ESPRESSO, FEROS, HARPS, and
Magellan
/PFS. We also incorporate
TESS
observations of the warm Saturn–hosting systems HATS-47 (a.k.a. TOI 1073.01), HATS-48A, and HATS-49. HATS-47 was independently identified as a candidate by the
TESS
team, while the other two systems were not previously identified from the
TESS
data. The RV orbital variations are measured for these systems using
Magellan
/PFS. HATS-48A has a resolved
neighbor in
Gaia
DR2, which is a common-proper-motion binary star companion to HATS-48A with a mass of 0.22
and a current projected physical separation of ∼1400 au.
We report the discovery of a Jupiter-size planet transiting a relatively bright (V = 11.56) and metal-rich early K dwarf star with a period of similar to 2.9 days. On the basis of follow-up ...photometry and spectroscopy we determine the mass and radius of the planet, HAT-P-3b, to be M sub(p) = 0.599 plus or minus 0.026 M sub(Jap) and R sub(p) = 0.890 plus or minus 0.046 R sub(Jap). The relatively small size of the object for Its mass implies the presence of about 75 M unk worth of heavy elements ( similar to unk4 of the total mass) based on current theories of Irradiated extrasolar giant planets, similar to the mass of the core inferred for the transiting planet HD 149026b. The bulk density of HAT-P-3b is found to be rho p = 1.06 plus or minus 0-17 g cm sub(-3), and the planet orbits the star at a distance of 0.03894 AU. Ephemerides for the transit centers are T sub(c) = 2.454, 218.7594 plus or minus 0.0029 + N x (2.899703 plus or minus 0.000054) (HJD).
We describe the discovery of HAT-P-4b, a low-density extrasolar planet transiting BD + 36 2593, a upsilon = 11.2 mag slightly evolved metal-rich late F star. The planet's orbital period is 3.056536 ...plus or minus 0.000057 days with a midtransit epoch of 2,454, 245.8154 plus or minus 0.0003 (HJD). Based on high-precision photometric and spectroscopic data, and by using transit light curve modeling, spectrum analysis, and evolutionary models, we derive the following planet parameters: unk = 0.68 plus or minus 0.04 unk, unk = 1.27 plus or minus 0.05 unk, unk= 0.41 plus or minus 0.06 sub(g)cm super(-3), and unk= 0.0446 plus or minus 0.0012 AU. Because of its relatively large radius, together with its assumed high metallicity (that of its parent star), this planet adds to the theoretical challenges of explaining inflated extrasolar planets.
Goldfish production increase in four years, specifically 66,823,000 in 2010 to 72,997,000 in 2014. The increment of goldfish production growth altogether with problems which is a discontinuity of fry ...stock. The solution for this problem is the purpose of this study, which is understood techniques in Goldfish (Carassius auratus) hatchery. The feed given to goldfish brood is blood worms (Chironomus sp. larvae) and pellets with a ratio of 50:50 as much as 3% of the biomass. Goldfish hatchery techniques involve broodstock cultivation, spawning techniques, larval development observation, and larval cultivation. Two kinds of Goldfish used, namely Oranda and Mutiara Goldfish. The results of Oranda goldfish spawning and Mutiara goldfish spawning consecutively are Fecundity 875 eggs, FR 94%, HR 91.83%, SR 93.04% and Fecundity 3850 eggs, FR 93.66%, HR 92.48%, and SR 91.10%. Larval development observation includes embryogenesis until post-hatched larval. Larval cultivation consists of giving various types of feeds, which are artemia nauplii (for 3-7 days old larval), Moina (for 7-14 days old larval), and blood worm or tubifex (> 14 days old larval). Fertilized goldfish eggs will develop through several phases, including zygotes, initial cleavage, blastula, gastrula, segmentation, pharyngula, egg hatching, and development of larvae after hatching.
We report the discovery of HAT-P-15b, a transiting extrasolar planet in the 'period valley,' a relatively sparsely populated period regime of the known extrasolar planets. The host star, GSC ...2883-01687, is a G5 dwarf with V= 12.16. It has a mass of 1.01 ? 0.04 M , radius of 1.08 ? 0.04 R , effective temperature 5568 ? 90 K, and metallicity Fe/H = +0.22 ? 0.08. The planetary companion orbits the star with a period P = 10.863502 ? 0.000027 days, transit epoch Tc = 2454638.56019 ? 0.00048 (BJD), and transit duration 0.2285 ? 0.0015 days. It has a mass of 1.946 ? 0.066 M J and radius of 1.072 ? 0.043 R J yielding a mean density of 1.96 ? 0.22 g cm-3. At an age of 6.8+2.5 --1.6 Gyr, the planet is H/He-dominated and theoretical models require about 2% (10 M {circled plus}) worth of heavy elements to reproduce its measured radius. With an estimated equilibrium temperature of ~820 K during transit, and ~1000 K at occultation, HAT-P-15b is a potential candidate to study moderately cool planetary atmospheres by transmission and occultation spectroscopy.
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