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Journal articles on the topic 'Solar energy photometry'

Author: Grafiati

Published: 6 September 2023

Last updated: 31 July 2025

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1

Sobotka, M., M. Vázquez, M. Sánchez Cuberes, J. A. Bonet, and A. Hanslmeier. "Infrared Photometry of Solar Active Regions." International Astronomical Union Colloquium 179 (2000): 289–92. http://dx.doi.org/10.1017/s0252921100064691.

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AbstractSimultaneous time series of broad-band images of two active regions close to the disk center were acquired at the maximum (0.80μm) and minimum (1.55μm) continuum opacities. Dark faculae are detected in images obtained as weighted intensity differences between both wavelength bands. The elements of quiet regions can be clearly distinguished from those of faculae and pores in scatter plots of brightness temperatures. There is a smooth transition between faculae and pores in the scatter plots. These facts are interpreted in terms of the balance between the inhibition of convective energy

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Glushneva, I. N., E. A. Markova, and A. V. Kharitonov. "Energy Distribution, Photometry and Physical Characteristics of the Sun and Solar Analogs." Highlights of Astronomy 7 (1986): 853–61. http://dx.doi.org/10.1017/s1539299600007383.

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AbstractColor indices of solar analogs in the Vilnius seven-color photometric system are discussed. The physical parameters (effective temperatures, radii and luminosities) for solar analogs with reliable spectrophotometric and photometric data were obtained by means of infrared fluxes. The effective temperatures of 16 Cyg A and B, which are considered to be the closest solar analogs are 5854 and 5664 K, respectively. The radii of both stars are in the range of 1 Ro < R < 1.4 Ro and luminosities 1.2Lo < L < 2.1 Lo for 16 Cyg A and Lo < L < 1.7 Lo for 16 Cyg B depending on dif

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Zhi, Hui, Xiaojun Jiang, and Jianfeng Wang. "Multicolour photometry of LEO mega-constellations Starlink and OneWeb." Monthly Notices of the Royal Astronomical Society 530, no. 4 (2024): 5006–15. http://dx.doi.org/10.1093/mnras/stae693.

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ABSTRACT The development of low earth orbit (LEO) mega-constellation fundamentally threatens ground-based optical astronomical observations. To study the photometric properties of the LEO mega-constellations, we used the Xinglong 50 cm telescope to conduct a large-sample, high-precision, and multicolour target-tracking photometry of two typical LEO mega-constellations: Starlink and OneWeb. Over a three-month observation period starting on 2022 January 1, we collected 1447 light curves of 404 satellites in four typical versions: Starlink v1.0, DarkSat, VisorSat, Starlink v1.5, and OneWeb. Accor

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Maehara, Hiroyuki. "Starspot Activity and Superflares on Solar-type Stars." Proceedings of the International Astronomical Union 12, S328 (2016): 22–29. http://dx.doi.org/10.1017/s1743921317003945.

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AbstractRecent high-precision photometry from space (e.g., Kepler) enables us to investigate the nature of “superflares” on solar-type stars. The bolometric energy of superflares detected by Kepler ranges from 1033 erg to 1036 erg which is 10-10,000 times larger than that released by a typical X10 class solar flare. The occurrence frequency (dN/dE) of superflares as a function of flare energy (E) shows the power-law distribution with the power-law index of ~−1.8 for 1034 < E < 1036 erg. Most of superflare stars show quasi-periodic light variations which suggest the presence of large star

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Carry, B. "Solar system science with ESA Euclid." Astronomy & Astrophysics 609 (January 2018): A113. http://dx.doi.org/10.1051/0004-6361/201730386.

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Context. The ESA Euclid mission has been designed to map the geometry of the dark Universe. Scheduled for launch in 2020, it will conduct a six-year visible and near-infrared imaging and spectroscopic survey over 15 000 deg2 down to VAB ~ 24.5. Although the survey will avoid ecliptic latitudes below 15°, the survey pattern in repeated sequences of four broadband filters seems well-adapted to detect and characterize solar system objects (SSOs). Aims. We aim at evaluating the capability of Euclid of discovering SSOs and of measuring their position, apparent magnitude, and spectral energy distrib

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Durbin, M. J., R. L. Beaton, A. J. Monson, B. Swidler, and J. J. Dalcanton. "Empirical 2MASS–WFC3/IR Filter Transformations Across the H-R Diagram from Synthetic Photometry." Astronomical Journal 166, no. 6 (2023): 236. http://dx.doi.org/10.3847/1538-3881/acfaa1.

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Abstract Near-infrared bandpasses on spaceborne observatories diverge from their ground-based counterparts as they are free of atmospheric telluric absorption. Available transformations between respective filter systems in the literature rely on theoretical stellar atmospheres, which are known to have difficulties reproducing the observed spectral energy distributions of cool giants. We present new transformations between the Two Micron All Sky Survey JHK S and Hubble Space Telescope WFC3/IR F110W, F125W, and F160W photometric systems based on synthetic photometry of empirical stellar spectra

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Bernardinelli, Pedro H., Gary M. Bernstein, Nicholas Jindal, et al. "Photometry of Outer Solar System Objects from the Dark Energy Survey. I. Photometric Methods, Light-curve Distributions, and Trans-Neptunian Binaries." Astrophysical Journal Supplement Series 269, no. 1 (2023): 18. http://dx.doi.org/10.3847/1538-4365/acf6bf.

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Abstract We report the methods of and initial scientific inferences from the extraction of precision photometric information for the >800 trans-Neptunian objects (TNOs) discovered in the images of the Dark Energy Survey (DES). Scene-modeling photometry is used to obtain shot-noise-limited flux measures for each exposure of each TNO, with background sources subtracted. Comparison of double-source fits to the pixel data with single-source fits are used to identify and characterize two binary TNO systems. A Markov Chain Monte Carlo method samples the joint likelihood of the intrinsic colors of

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Kim, I. S., N. L. Kroussanova, O. T. Matsuura, et al. "Using color photometry to search for the solar corona “reddening” effect." Radiophysics and Quantum Electronics 39, no. 10 (1996): 862–64. http://dx.doi.org/10.1007/bf02120975.

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Lipunov, Vladimir, Victor Kornilov, Evgeny Gorbovskoy, et al. "Master Robotic Net." Advances in Astronomy 2010 (2010): 1–6. http://dx.doi.org/10.1155/2010/349171.

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The main goal of the MASTER-Net project is to produce a unique fast sky survey with all sky observed over a single night down to a limiting magnitude of 19-20. Such a survey will make it possible to address a number of fundamental problems: search for dark energy via the discovery and photometry of supernovae (including SNIa), search for exoplanets, microlensing effects, discovery of minor bodies in the Solar System, and space-junk monitoring. All MASTER telescopes can be guided by alerts, and we plan to observe prompt optical emission from gamma-ray bursts synchronously in several filters and

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Vasilyev, Valeriy, Timo Reinhold, Alexander I. Shapiro, et al. "Sun-like stars produce superflares roughly once per century." Science 386, no. 6727 (2024): 1301–5. https://doi.org/10.1126/science.adl5441.

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Stellar superflares are energetic outbursts of electromagnetic radiation that are similar to solar flares but release more energy, up to 10 36 erg on main-sequence stars. It is unknown whether the Sun can generate superflares and, if so, how often they might occur. We used photometry from the Kepler space observatory to investigate superflares on other stars with Sun-like fundamental parameters. We identified 2889 superflares on 2527 Sun-like stars, out of 56,450 observed. This detection rate indicates that superflares with energies >10 34 erg occur roughly once per century on stars with Su

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Han, Hyun-Joo, Muhammad Uzair Mehmood, Jin-Chul Park, Joo-Won Lee, Sang-Hoon Lim, and Seung-Jin Oh. "Identifying the Photometric Characteristics and Applicability of Hybrid Solar Lighting." Energies 15, no. 22 (2022): 8356. http://dx.doi.org/10.3390/en15228356.

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The present research aims at promoting the stability and applicability of a hybrid daylighting system combining daylight and artificial light, which eventually enables a constant and pleasant luminous flux of the mixed light delivered by a terminal device installed indoors. That is, the present system allows a constant amount of luminous flux through its terminal device similar to an electric lamp, demonstrating its energy efficiency as well as comfortableness. The system effectively combines two different types of light, as solar rays are collected by a solar tracking sun light collector. The

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De, K., M. M. Kasliwal, E. O. Ofek, et al. "A hot and fast ultra-stripped supernova that likely formed a compact neutron star binary." Science 362, no. 6411 (2018): 201–6. http://dx.doi.org/10.1126/science.aas8693.

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Compact neutron star binary systems are produced from binary massive stars through stellar evolution involving up to two supernova explosions. The final stages in the formation of these systems have not been directly observed. We report the discovery of iPTF 14gqr (SN 2014ft), a type Ic supernova with a fast-evolving light curve indicating an extremely low ejecta mass (≈0.2 solar masses) and low kinetic energy (≈2 × 1050ergs). Early photometry and spectroscopy reveal evidence of shock cooling of an extended helium-rich envelope, likely ejected in an intense pre-explosion mass-loss episode of t

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Bouvier, Jérôme, and Patrice Corporon. "Herbig Ae/Be Visual Binaries." Symposium - International Astronomical Union 200 (2001): 155–64. http://dx.doi.org/10.1017/s0074180900225175.

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We present the results of a high-angular resolution spectro-imaging survey of a sample of isolated Herbig Ae-Be (HAeBe) stars aimed at searching for close companions. The fraction of wide binaries is found to be significantly higher in HAeBe stars than in solar-mass field dwarfs, and suggests a companion star fraction possibly larger than 1. The spectral energy distribution of the primaries and secondaries is derived independently from multi-wavelength resolved photometry of the systems. It is found that young low-mass companions usually do not exhibit infrared excesses, which suggests that th

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Medina, Amber A., David Charbonneau, Jennifer G. Winters, Jonathan Irwin та Jessica Mink. "Variability Timescales of Hα on Active Mid-to-late M dwarfs". Astrophysical Journal 928, № 2 (2022): 185. http://dx.doi.org/10.3847/1538-4357/ac5738.

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Abstract We present a study of the variation timescales of the chromospheric activity indicator Hα on a sample of 13 fully convective, active mid-to-late M stars with masses between 0.1 and 0.3 solar masses. Our goal was to determine the dominant variability timescale and, by inference, a possible mechanism responsible for the variation. We gathered 10 or more high-resolution spectra each of 10 stars using the TRES spectrograph at times chosen to span all phases of stellar rotation, as determined from photometric data from the MEarth Observatories. All stars varied in their Hα emission. For ni

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Ayres, Thomas, and Derek Buzasi. "In the Trenches of the Solar–Stellar Connection. VI. Total EclipSS." Astrophysical Journal Supplement Series 263, no. 2 (2022): 41. http://dx.doi.org/10.3847/1538-4365/ac8cfc.

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Abstract The Ecliptic poles Stellar Survey (EclipSS; 2018–2019) collected Hubble Space Telescope/Cosmic Origins Spectrograph (COS) 1150–1420 Å spectra of 49 FGK dwarfs at high ecliptic latitudes. These regions are favored by the scanning programs of the Transiting Exoplanet Survey Satellite (TESS; high-precision optical light curves) and Extended Roentgen Survey with an Imaging Telescope Array (eROSITA; repeated X-ray visits over half a decade), which can provide vital ancillary support in the exploration of high-energy “stellar activity.” The present study is a follow-on, focused on new Chand

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Duval-Poo, M. A., M. Piana, and A. M. Massone. "Solar hard X-ray imaging by means of compressed sensing and finite isotropic wavelet transform." Astronomy & Astrophysics 615 (July 2018): A59. http://dx.doi.org/10.1051/0004-6361/201731765.

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Aims. Compressed sensing realized by means of regularized deconvolution and the finite isotropic wavelet transform is effective and reliable in hard X-ray solar imaging. Methods. The method uses the finite isotropic wavelet transform with the Meyer function as the mother wavelet. Furthermore, compressed sensing is realized by optimizing a sparsity-promoting regularized objective function by means of the fast iterative shrinkage-thresholding algorithm. Eventually, the regularization parameter is selected by means of the Miller criterion. Results. The method is applied against both synthetic dat

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Beskin, G. M., S. I. Neizvestnyj, V. L. Plakhotnichenko, L. A. Pustil'nik, V. F. Shvartsman, and R. E. Gershberg. "High Time Resolution Photometry of Red Dwarf Flare Stars III. The Most Rapid and Faintest Observed Stellar Flares; their Physics and Statistics." International Astronomical Union Colloquium 104, no. 2 (1989): 103–5. http://dx.doi.org/10.1017/s0252921100153916.

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AbstractHigh time resolution monitoring of the UV Cet type flare stars has enabled as to detect flares with total duration of a few seconds and with energy output comparable to solar subflares. We find that the time scales of decay for such flares correspond to recombination times of optically thin gas or to cooling times of optically thick gas heated in flares. Therefore, faster flares cannot be detected individually but their accumulated effect may be one source of brightness fluctuations of the “quiet” star. The upper limit for the total power of such microflares does not exceed the time-av

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Shivaei, Irene, Gergö Popping, George Rieke, et al. "Infrared Spectral Energy Distributions and Dust Masses of Sub-solar Metallicity Galaxies at z ∼ 2.3." Astrophysical Journal 928, no. 1 (2022): 68. http://dx.doi.org/10.3847/1538-4357/ac54a9.

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Abstract We present results from Atacama Large Millimeter/submillimeter Array (ALMA) 1.2 mm continuum observations of a sample of 27 star-forming galaxies at z = 2.1–2.5 from the MOSFIRE Deep Evolution Field survey with metallicity and star formation rate measurements from optical emission lines. Using stacks of Spitzer, Herschel, and ALMA photometry (rest frame ∼8–400 μm), we examine the infrared (IR) spectral energy distributions (SED) of z ∼ 2.3 subsolar-metallicity (∼0.5 Z ⊙) luminous infrared galaxies (LIRGs). We find that the data agree well with an average template of higher-luminosity

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Tristan, Isaiah I., Yuta Notsu, Adam F. Kowalski, et al. "A 7 Day Multiwavelength Flare Campaign on AU Mic. I. High-time-resolution Light Curves and the Thermal Empirical Neupert Effect." Astrophysical Journal 951, no. 1 (2023): 33. http://dx.doi.org/10.3847/1538-4357/acc94f.

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Abstract We present light curves and flares from a 7 day, multiwavelength observational campaign of AU Mic, a young and active dM1e star with exoplanets and a debris disk. We report on 73 unique flares between the X-ray to optical data. We use high-time-resolution near-UV (NUV) photometry and soft X-ray (SXR) data from the X-ray Multi-Mirror Mission to study the empirical Neupert effect, which correlates the gradual and impulsive phase flaring emissions. We find that 65% (30 of 46) flares do not follow the Neupert effect, which is 3 times more excursions than seen in solar flares, and propose

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Beiler, Samuel A., Michael C. Cushing, J. Davy Kirkpatrick, et al. "Precise Bolometric Luminosities and Effective Temperatures of 23 Late-T and Y Dwarfs Obtained with JWST." Astrophysical Journal 973, no. 2 (2024): 107. http://dx.doi.org/10.3847/1538-4357/ad6301.

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Abstract We present infrared spectral energy distributions of 23 late-type T and Y dwarfs obtained with the James Webb Space Telescope. The spectral energy distributions consist of NIRSpec PRISM and MIRI low-resolution spectrometer spectra covering the ∼1–12 μm wavelength range at λ/Δλ ≈ 100 and broadband photometry at 15, 18, and 21 μm. The spectra exhibit absorption features common to these objects including H2O, CH4, CO, CO2, and NH3. Interestingly, while the spectral morphology changes relatively smoothly with spectral type at λ < 3 μm and λ > 8 μm, it shows no clear trend in the 5 μ

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Bernardinelli, Pedro H., Gary M. Bernstein, T. M. C. Abbott, et al. "Photometry of Outer Solar System Objects from the Dark Energy Survey. II. A Joint Analysis of Trans-Neptunian Absolute Magnitudes, Colors, Light Curves and Dynamics." Astronomical Journal 169, no. 6 (2025): 305. https://doi.org/10.3847/1538-3881/adc459.

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Abstract For the 696 trans-Neptunian objects (TNOs) with absolute magnitudes 5.5 < H r < 8.2 detected in the Dark Energy Survey, we characterize the relationships between their dynamical state and physical properties—namely H r , indicating size; colors, indicating surface composition; and flux variation semiamplitude A, indicating asphericity and surface inhomogeneity. We seek “birth” physical distributions that can recreate these parameters in every dynamical class. We show that the observed colors of these TNOs are consistent with two Gaussian distributions in griz space, “near-infrar

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Kanodia, Shubham, Jessica Libby-Roberts, Caleb I. Cañas, et al. "TOI-3757 b: A Low-density Gas Giant Orbiting a Solar-metallicity M Dwarf." Astronomical Journal 164, no. 3 (2022): 81. http://dx.doi.org/10.3847/1538-3881/ac7c20.

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Abstract We present the discovery of a new Jovian-sized planet, TOI-3757 b, the lowest-density transiting planet known to orbit an M dwarf (M0V). This planet was discovered around a solar-metallicity M dwarf, using Transiting Exoplanet Survey Satellite photometry and confirmed with precise radial velocities from the Habitable-zone Planet Finder (HPF) and NEID. With a planetary radius of 12.0 − 0.5 + 0.4 R ⊕ and mass of 85.3 − 8.7 + 8.8 M ⊕, not only does this object add to the small sample of gas giants (∼10) around M dwarfs, but also its low density ( ρ = 0.27 − 0.04 + 0.05 g cm−3) provides a

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Puga, E., C. Neiner, S. Hony, A. Lenorzer, A. M. Hubert, and L. B. F. M. Waters. "Massive star formation in the outer Galaxy: S284." Proceedings of the International Astronomical Union 2, S237 (2006): 465. http://dx.doi.org/10.1017/s1743921307002530.

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AbstractS284 is a diffuse HII region located in the anti-centre of the galactic disk (l=212, b=−1.3), at a distance of 5.5 kpc and it is relatively isolated. S284 harbours a cluster of stars in its centre known as Dolidze 25 (also known as C 0642+0.03). A spectroscopic study of the cluster sources (Lennon et al. 1990, A&A, 240, 349) revealed: a) the spectral types of these central sources and b) the low metallicity of the cluster (a factor six lower than the solar metallicity). The age of the cluster (6 Myr) has been determined through isochrone fitting of precision photometry (Turbide &am

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Ilin, Ekaterina, Sarah J. Schmidt, James R. A. Davenport, and Klaus G. Strassmeier. "Flares in open clusters with K2." Astronomy & Astrophysics 622 (February 2019): A133. http://dx.doi.org/10.1051/0004-6361/201834400.

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Context. The presence and strength of a stellar magnetic field and activity is rooted in a star’s fundamental parameters such as mass and age. Can flares serve as an accurate stellar “clock”? Aims. To explore if we can quantify an activity-age relation in the form of a flaring-age relation, we measured trends in the flaring rates and energies for stars with different masses and ages. Methods. We investigated the time-domain photometry provided by Kepler’s follow-up mission K2 and searched for flares in three solar metallicity open clusters with well-known ages, M 45 (0.125 Gyr), M 44 (0.63 Gyr

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Meza, Nicolás, J. L. Prieto, A. Clocchiatti, et al. "The extraplanar type II supernova ASASSN-14jb in the nearby edge-on galaxy ESO 467-G051." Astronomy & Astrophysics 629 (September 2019): A57. http://dx.doi.org/10.1051/0004-6361/201834972.

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We present optical photometry and spectroscopy of the Type II supernova ASASSN-14jb, together with Very Large Telescope (VLT) Multi Unit Spectroscopic Explorer (MUSE) integral field observations of its host galaxy and a nebular-phase spectrum. This supernova, in the nearby galaxy ESO 467-G051 (z = 0.006), was discovered and followed-up by the all-sky automated survey for supernovae (ASAS-SN). We obtained well-sampled las cumbres network (LCOGTN) BVgri and Swift w2m1w1ubv optical, near-UV/optical light curves, and several optical spectra in the early photospheric phases. The transient ASASSN-14

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Miret-Roig, N., N. Huélamo, and H. Bouy. "Searching for debris discs in the 30 Myr open cluster IC 4665." Astronomy & Astrophysics 641 (September 2020): A156. http://dx.doi.org/10.1051/0004-6361/202038205.

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Context. Debris discs orbiting young stars are key to understanding dust evolution and the planetary formation process. We take advantage of a recent membership analysis of the 30 Myr nearby open cluster IC 4665 based on the Gaia and DANCe surveys to revisit the disc population of this cluster. Aims. We aim to study the disc population of IC 4665 using Spitzer (MIPS and IRAC) and WISE photometry. Methods. We use several colour–colour diagrams with empirical photospheric sequences to detect the sources with an infrared excess. Independently, we also fit the spectral energy distribution (SED) of

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Osborne, Chandler, and Samir Salim. "Strategies for Obtaining Robust Spectral Energy Distribution Fitting Parameters for Galaxies at z ∼ 1 and z ∼ 2 in the Absence of Infrared Data." Astrophysical Journal 962, no. 1 (2024): 59. http://dx.doi.org/10.3847/1538-4357/ad17c8.

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Abstract Robust estimation of star formation rates (SFRs) at higher redshifts (z ≳ 1) using UV–optical–near-infrared (NIR) photometry is contingent on the ability of spectral energy distribution (SED) fitting to constrain the dust attenuation, stellar metallicity, and star formation history (SFH) simultaneously. IR-derived dust luminosities can help break the degeneracy between these parameters, but IR data are often not available. Here, we explore strategies for SED fitting at z ≳ 1 in the absence of IR data using a sample of log M * > 10.2 star-forming galaxies from the Cosmic Assembly Ne

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Geier, S. J., K. E. Heintz, J. P. U. Fynbo та ін. "Gaia-assisted selection of a quasar reddened by dust in an extremely strong damped Lyman-α absorber at z = 2.226". Astronomy & Astrophysics 625 (травень 2019): L9. http://dx.doi.org/10.1051/0004-6361/201935108.

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Damped Lyman-α absorbers (DLAs) as a class of quasi-stellar object (QSO) absorption-line systems are currently our most important source of detailed information on the cosmic chemical evolution of galaxies. However, the degree to which this information is biased by dust remains to be understood. One strategy is to specifically search for QSOs that are reddened by metal-rich and dusty foreground absorbers. In this Letter, we present the discovery of a z = 2.60 QSO that is strongly reddened by dust in an intervening extremely strong DLA at z = 2.226. This QSO was identified through a novel selec

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Mattila, K., M. Haas, L. K. Haikala, et al. "Optical and UV surface brightness of translucent dark nebulae." Astronomy & Astrophysics 617 (September 2018): A42. http://dx.doi.org/10.1051/0004-6361/201833196.

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Context. Dark nebulae display a surface brightness because dust grains scatter light of the general interstellar radiation field (ISRF). High-galactic-latitudes dark nebulae are seen as bright nebulae when surrounded by transparent areas which have less scattered light from the general galactic dust layer. Aims. Photometry of the bright dark nebulae LDN 1780, LDN 1642, and LBN 406 shall be used to derive scattering properties of dust and to investigate the presence of UV fluorescence emission by molecular hydrogen and the extended red emission (ERE). Methods. We used multi-wavelength optical p

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Madore, Barry F., Wendy L. Freedman, and Kayla Owens. "Chicago–Carnegie Hubble Program: A Multiwavelength Search for the Effects of Metallicity on the Cepheid Distance Scale. II. Theoretical Models and Synthetic Spectra." Astrophysical Journal 981, no. 1 (2025): 32. https://doi.org/10.3847/1538-4357/ada3d5.

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Abstract This is the second of two papers exploring the effects of metallicity on the multiwavelength properties of Cepheids in terms of their multiwavelength period–luminosity (PL) relations, impacting their use as extragalactic distance indicators and underpinning one of the most popular paths to estimating the expansion rate of the Universe, H 0. In Paper I, we presented five tests for the influence of metallicity on galactic and extragalactic Cepheid PL relations, spanning nearly 2 dex in metallicity and inspecting PL relations from the optical (BVI), through the near-infrared (JHK), and i

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Foote, Trevor O., Nikole K. Lewis, Brian M. Kilpatrick, et al. "The Emission Spectrum of the Hot Jupiter WASP-79b from HST/WFC3." Astronomical Journal 163, no. 1 (2021): 7. http://dx.doi.org/10.3847/1538-3881/ac2f4a.

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Abstract Here we present a thermal emission spectrum of WASP-79b, obtained via Hubble Space Telescope Wide Field Camera 3 G141 observations as part of the PanCET program. As we did not observe the ingress or egress of WASP-79b’s secondary eclipse, we consider two scenarios: a fixed mid-eclipse time based on the expected occurrence time, and a mid-eclipse time as a free parameter. In both scenarios, we can measure thermal emission from WASP-79b from 1.1 to 1.7 μm at 2.4σ confidence consistent with a 1900 K brightness temperature for the planet. We combine our observations with Spitzer dayside p

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Delorme, P., T. Dupuy, J. Gagné, et al. "CFBDSIR 2149-0403: young isolated planetary-mass object or high-metallicity low-mass brown dwarf?" Astronomy & Astrophysics 602 (June 2017): A82. http://dx.doi.org/10.1051/0004-6361/201629633.

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Aims. We conducted a multi-wavelength, multi-instrument observational characterisation of the candidate free-floating planet CFBDSIR J214947.2−040308.9, a late T-dwarf with possible low-gravity features, in order to constrain its physical properties. Methods. We analysed nine hours of X-shooter spectroscopy with signal detectable from 0.8 to 2.3 μm, as well as additional photometry in the mid-infrared using the Spitzer Space Telescope. Combined with a VLT/HAWK-I astrometric parallax, this enabled a full characterisation of the absolute flux from the visible to 5 μm, encompassing more than 90%

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Ivezić, Željko, J. Anthony Tyson, Mario Jurić, et al. "LSST: Comprehensive NEO detection, characterization, and orbits." Proceedings of the International Astronomical Union 2, S236 (2006): 353–62. http://dx.doi.org/10.1017/s1743921307003420.

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AbstractThe Large Synoptic Survey Telescope (LSST) is currently by far the most ambitious proposed ground-based optical survey. With initial funding from the National Science Foundation (NSF), Department of Energy (DOE) laboratories, and private sponsors, the design and development efforts are well underway at many institutions, including top universities and national laboratories. Solar System mapping is one of the four key scientific design drivers, with emphasis on efficient Near-Earth Object (NEO) and Potentially Hazardous Asteroid (PHA) detection, orbit determination, and characterization

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Zhang, Yun-Jin, A.-Li Luo, Biwei Jiang, et al. "Identification and Parameter Determination of F-type Herbig Stars from LAMOST DR8." Astrophysical Journal 936, no. 2 (2022): 151. http://dx.doi.org/10.3847/1538-4357/ac84da.

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Abstract We identify 20 F-type Herbig stars and provide a list of 22 pre-main-sequence candidates from LAMOST DR8. The effective temperature, distance, extinction, stellar luminosity, mass, age, and radius are derived for each Herbig star based on optical spectra, photometry, Gaia EDR3 parallaxes, and pre-main-sequence evolutionary tracks. According to spectral energy distribution, 19 F-type Herbig stars belong to Class II YSOs, and one belongs to the flat-spectrum class. Four have Spitzer IRS spectra, of which three show extremely weak polycyclic aromatic hydrocarbon emissions, and three with

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Vaičiulytė, Vaida, Kristina Ložienė, and Ričardas Taraškevičius. "Impact of Edaphic and Climatic Factors on Thymus pulegioides Essential Oil Composition and Potential Prevalence of Chemotypes." Plants 11, no. 19 (2022): 2536. http://dx.doi.org/10.3390/plants11192536.

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Intraspecific chemical polymorphism is characteristic of essential oil bearing Thymus pulegioides (Lamiaceae). Soil chemical composition and climatic conditions can influence not only quantitative and qualitative composition of essential oils, but also on prevalence of different chemotypes in space. The purpose of study was to determine the impact of edaphic and climatic factors on T. pulegioides essential oil composition and potential chemotypes prevalence. It were investigated 131 habitats of T. pulegioides in all ten climatic sub-districts of Lithuania. Essential oils were isolated by hydro

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Parrag, Eleonora, Cosimo Inserra, Steve Schulze, et al. "SN 2019hcc: a Type II supernova displaying early O ii lines." Monthly Notices of the Royal Astronomical Society 506, no. 4 (2021): 4819–40. http://dx.doi.org/10.1093/mnras/stab2074.

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ABSTRACT We present optical spectroscopy together with ultraviolet, optical, and near-infrared photometry of SN 2019hcc, which resides in a host galaxy at redshift 0.044, displaying a sub-solar metallicity. The supernova spectrum near peak epoch shows a ‘w’ shape at around 4000 Å which is usually associated with O ii lines and is typical of Type I superluminous supernovae. SN 2019hcc post-peak spectra show a well-developed H α P-Cygni profile from 19 d past maximum and its light curve, in terms of its absolute peak luminosity and evolution, resembles that of a fast-declining Hydrogen-rich supe

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Fensch, Jérémy, Pierre-Alain Duc, Médéric Boquien, et al. "Massive star cluster formation and evolution in tidal dwarf galaxies." Astronomy & Astrophysics 628 (August 2019): A60. http://dx.doi.org/10.1051/0004-6361/201834403.

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Context. The formation of globular clusters remains an open debate. Dwarf starburst galaxies are efficient at forming young massive clusters with similar masses as globular clusters and may hold the key to understanding their formation. Aims. We study star cluster formation in a tidal debris, including the vicinity of three tidal dwarf galaxies, in a massive gas-dominated collisional ring around NGC 5291. These dwarfs have physical parameters that differ significantly from local starbursting dwarfs. They are gas rich, highly turbulent, their gas metallicity is already enriched up to half solar

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Naidu, Rohan P., Pascal A. Oesch, Pieter van Dokkum, et al. "Two Remarkably Luminous Galaxy Candidates at z ≈ 10–12 Revealed by JWST." Astrophysical Journal Letters 940, no. 1 (2022): L14. http://dx.doi.org/10.3847/2041-8213/ac9b22.

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Abstract The first few 100 Myr at z > 10 mark the last major uncharted epoch in the history of the universe, where only a single galaxy (GN-z11 at z ≈ 11) is currently spectroscopically confirmed. Here we present a search for luminous z > 10 galaxies with JWST/NIRCam photometry spanning ≈1–5 μm and covering 49 arcmin2 from the public JWST Early Release Science programs (CEERS and GLASS). Our most secure candidates are two M UV ≈ −21 systems: GLASS-z12 and GLASS-z10. These galaxies display abrupt ≳1.8 mag breaks in their spectral energy distributions (SEDs), consistent with complete absor

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Groenewegen, M. A. T. "A WISE view on extreme AGB stars." Astronomy & Astrophysics 659 (March 2022): A145. http://dx.doi.org/10.1051/0004-6361/202142648.

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Context. Variability is a key property of stars on the asymptotic giant branch (AGB). Their pulsation period is related to the luminosity and mass-loss rate (MLR) of the star. Long-period variables (LPVs) and Mira variables are the most prominent of all types of variability of evolved stars. However, the reddest, most obscured AGB stars are too faint in the optical and have eluded large variability surveys. Aims. Our goal is to obtain a sample of LPVs with large MLRs by analysing WISE W1 and W2 light curves (LCs) for about 2000 sources, photometrically selected to include known C-stars with th

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Levy, R. C., L. A. Remer, J. V. Martins, et al. "Evaluation of the MODIS Aerosol Retrievals over Ocean and Land during CLAMS." Journal of the Atmospheric Sciences 62, no. 4 (2005): 974–92. http://dx.doi.org/10.1175/jas3391.1.

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Abstract The Chesapeake Lighthouse Aircraft Measurements for Satellites (CLAMS) experiment took place from 10 July to 2 August 2001 in a combined ocean–land region that included the Chesapeake Lighthouse [Clouds and the Earth’s Radiant Energy System (CERES) Ocean Validation Experiment (COVE)] and the Wallops Flight Facility (WFF), both along coastal Virginia. This experiment was designed mainly for validating instruments and algorithms aboard the Terra satellite platform, including the Moderate Resolution Imaging Spectroradiometer (MODIS). Over the ocean, MODIS retrieved aerosol optical depths

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Mrozek, Tomasz, Szymon Gburek, Marek Siarkowski, et al. "Solar flares observed simultaneously with SphinX, GOES and RHESSI." Proceedings of the International Astronomical Union 8, S294 (2012): 571–72. http://dx.doi.org/10.1017/s1743921313003256.

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AbstractIn February 2009, during recent deepest solar minimum, Polish Solar Photometer in X-rays (SphinX) begun observations of the Sun in the energy range of 1.2–15 keV. SphinX was almost 100 times more sensitive than GOES X-ray Sensors. The silicon PIN diode detectors used in the experiment were carefully calibrated on the ground using Synchrotron Radiation Source BESSY II. The SphinX energy range overlaps with the Ramaty High Energy Solar Spectroscopic Imager (RHESSI) energy range. The instrument provided us with observations of hundreds of very small flares and X-ray brightenings. We have

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Wood, John, Tim J. Smyth, and Victor Estellés. "Autonomous marine hyperspectral radiometers for determining solar irradiances and aerosol optical properties." Atmospheric Measurement Techniques 10, no. 5 (2017): 1723–37. http://dx.doi.org/10.5194/amt-10-1723-2017.

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Abstract. We have developed two hyperspectral radiometer systems which require no moving parts, shade rings or motorised tracking, making them ideally suited for autonomous use in the inhospitable remote marine environment. Both systems are able to measure direct and diffuse hyperspectral irradiance in the wavelength range 350–1050 nm at 6 nm (Spectrometer 1) or 3.5 nm (Spectrometer 2) resolution. Marine field trials along a 100° transect (between 50° N and 50° S) of the Atlantic Ocean resulted in close agreement with existing commercially available instruments in measuring (1) photosynthetica

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Gryciuk, Magdalena, Szymon Gburek, Marek Siarkowski, Piotr Podgorski, Janusz Sylwester, and Frantisek Farnik. "Comparison of solar activity during last two minima on turn of Activity Cycles 22/23 and 23/24." Proceedings of the International Astronomical Union 8, S294 (2012): 65–66. http://dx.doi.org/10.1017/s1743921313002226.

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AbstractThe subject of our work is the review and comparison of solar activity during the last two solar minima that occurred between recent activity cycles. We use the soft X-ray global solar corona observations covering the two nine-months long time intervals in 1997/98 and 2009. Data from RF15-I multichannel photometer are used for the penultimate minimum. For the last unusually deep and prolonged solar activity minimum in 2009 the data from SphinX spectrophotometer are used. Comparison of measurements from both minima takes place in the overlapping energy range 2–15 keV. We focus on the ac

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Neidig, Donald F. "The Importance of Solar White-Light Flares." International Astronomical Union Colloquium 104, no. 1 (1989): 261–69. http://dx.doi.org/10.1017/s0252921100031924.

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AbstractThe basic results of white-light flare (WLF) photometric and spectrographic observations are reviewed. WLFs represent the most extreme density conditions in solar optical flares and are similar to stellar flares in many respects. It is shown that WLFs originate in the low chromosphere and upper photosphere, and that their huge radiative losses remain difficult to explain within the context of known mechanisms of energy transport.

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Masoom, Akriti, Panagiotis Kosmopoulos, Ankit Bansal, and Stelios Kazadzis. "Solar Energy Estimations in India Using Remote Sensing Technologies and Validation with Sun Photometers in Urban Areas." Remote Sensing 12, no. 2 (2020): 254. http://dx.doi.org/10.3390/rs12020254.

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Solar radiation ground data is available in poor spatial resolution, which provides an opportunity and demonstrates the necessity to consider solar irradiance modeling based on satellite data. For the first time, solar energy monitoring in near real-time has been performed for India. This study focused on the assessment of solar irradiance from the Indian Solar Irradiance Operational System (INSIOS) using operational cloud and aerosol data from INSAT-3D and Copernicus Atmosphere Monitoring Service (CAMS)-Monitoring Atmospheric Composition Climate (MACC), respectively. Simulations of the global

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Dumka, Umesh Chandra, Panagiotis G. Kosmopoulos, Shantikumar S. Ningombam, and Akriti Masoom. "Impact of Aerosol and Cloud on the Solar Energy Potential over the Central Gangetic Himalayan Region." Remote Sensing 13, no. 16 (2021): 3248. http://dx.doi.org/10.3390/rs13163248.

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We examine the impact of atmospheric aerosols and clouds on the surface solar radiation and solar energy at Nainital, a high-altitude remote location in the central Gangetic Himalayan region (CGHR). For this purpose, we exploited the synergy of remote-sensed data in terms of ground-based AERONET Sun Photometer and satellite observations from the MODerate Resolution Imaging Spectroradiometer (MODIS) and the Meteosat Second Generation (MSG), with radiative transfer model (RTM) simulations and 1 day forecasts from the Copernicus Atmosphere Monitoring Service (CAMS). Clouds and aerosols are one of

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Pap, Judit M. "Long-term solar irradiance variability." Symposium - International Astronomical Union 181 (1997): 235–50. http://dx.doi.org/10.1017/s0074180900061180.

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Measurements of the solar energy throughout the solar spectrum and understanding its variability provide important information about the physical processes and structural changes in the solar interior and in the solar atmosphere. Solar irradiance measurements (both bolometric and at various wavelengths) over the last two decades have demonstrated that the solar radiative output changes with time as an effect of the waxing and waning solar activity. Although the overall pattern of the long-term variations is similar in the entire spectrum and at various wavelengths, being higher during high sol

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Dewitte, Steven, Jan Cornelis, and Mustapha Meftah. "Centennial Total Solar Irradiance Variation." Remote Sensing 14, no. 5 (2022): 1072. http://dx.doi.org/10.3390/rs14051072.

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Total Solar Irradiance (TSI) quantifies the solar energy received by the Earth and therefore is of direct relevance for a possible solar influence on climate change on Earth. We analyse the TSI space measurements from 1991 to 2021, and we derive a regression model that reproduces the measured daily TSI variations with a Root Mean Square Error (RMSE) of 0.17 W/m2. The daily TSI regression model uses the MgII core to wing ratio as a facular brightening proxy and the Photometric Sunspot Index (PSI) as a measure of sunspot darkening. We reconstruct the annual mean TSI backwards to 1700 based on th

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Pan, Jiaming, Hsing Wen Lin, David W. Gerdes, et al. "Photometric Properties of Jupiter Trojans Detected by the Dark Energy Survey." Planetary Science Journal 3, no. 12 (2022): 269. http://dx.doi.org/10.3847/psj/aca4d1.

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Abstract The Jupiter Trojans are a large group of asteroids that are coorbiting with Jupiter near its L4 and L5 Lagrange points. The study of Jupiter Trojans is crucial for testing different models of planet formation that are directly related to our understanding of solar system evolution. In this work, we select known Jupiter Trojans listed by the Minor Planet Center from the full six years data set (Y6) of the Dark Energy Survey (DES) to analyze their photometric properties. The DES data allow us to study Jupiter Trojans with a fainter magnitude limit than previous studies in a homogeneous

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Karoff, C., T. S. Metcalfe, B. T. Montet, et al. "Sounding stellar cycles with Kepler – III. Comparative analysis of chromospheric, photometric, and asteroseismic variability." Monthly Notices of the Royal Astronomical Society 485, no. 4 (2019): 5096–104. http://dx.doi.org/10.1093/mnras/stz782.

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ABSTRACT By combining ground-based spectrographic observations of variability in the chromospheric emission from Sun-like stars with the variability seen in their eigenmode frequencies, it is possible to relate the changes observed at the surfaces of these stars to the changes taking place in the interior. By further comparing this variability to changes in the relative flux from the stars, one can obtain an expression for how these activity indicators relate to the energy output from the stars. Such studies become very pertinent when the variability can be related to stellar cycles as they ca

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