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Статті в журналах з теми "Mass photometry"

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Автор: Grafiati

Опубліковано: 7 липня 2024

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1

Prokhorov, M. E., A. I. Zakharov, V. G. Moshkalev, N. L. Krusanova, and M. S. Tuchin. "Mass Computations of the Brightness of Stars in an Arbitrary Spectral Band." Астрономический журнал 100, no. 6 (June 1, 2023): 500–511. http://dx.doi.org/10.31857/s0004629923050092.

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The problem of calculating the brightness of an array of stars in an arbitrary photometric band, which is not the standard band of astronomical photometry, is considered from their multicolor photometry in some other photometric system. A similar problem is to transfer photometric measurements of stars from one multicolor photometric system to another. This task includes methods for calculating and comparing magnitudes, as well as merging photometric catalogs. The questions of choice of various zero-points of photometry and reduction of measurements for the atmosphere are considered. The issues of reducing the error of the proposed methods are discussed. The article is partly based on a report presented at the conference “Modern Stellar Astronomy-2022”, held at the Caucasian Mountain Observatory of the Sternberg State Astronomical Institute, Moscow State University, in November 8–10, 2022.

2

Sarrouh, Ghassan T. E., Adam Muzzin, Kartheik G. Iyer, Lamiya Mowla, Sunna Withers, Nicholas S. Martis, Roberto Abraham, et al. "Exposing Line Emission: The Systematic Differences of Measuring Galaxy Stellar Masses with JWST NIRCam Medium versus Wide Band Photometry." Astrophysical Journal Letters 967, no. 1 (May 1, 2024): L17. http://dx.doi.org/10.3847/2041-8213/ad43e8.

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Abstract Photometrically derived stellar masses are known to suffer from systematic uncertainties, particularly due to nebular emission contributions to the spectral energy distribution (SED). Using James Webb Space Telescope NIRCam imaging from the CAnadian NIRISS Unbiased Cluster Survey, we introduce a comparison study of photometrically derived redshifts and stellar masses based on two photometric catalogs of the same field spanning ∼0.4–4.5 μm: one consisting solely of wide band photometry, and another employing a combination of wide and medium band photometry. We find that ∼70% of likely line emitters have consistent photometric redshifts between both catalogs, with a median stellar mass difference between the two catalogs of <0.2 dex across all redshift bins. There are, however, a subset of galaxies (5% at z ∼ 2 up to 15% at z ∼ 6) where wide bands underestimate emission line strengths and infer older stellar populations, leading to median stellar mass differences of ∼0.7 dex. Examination of the SEDs for galaxies with inconsistent photometric redshifts shows this is caused by the inability of the wide bands to distinguish continuum emission from emission lines. Computing a stellar mass density with our sample, we find that it is potentially underestimated using wide band photometry by ∼10%–20% at z < 4, and potentially overestimated by as much as a factor of 2–3 at z > 5. These systematic differences caused by the poor spectral resolution of wide bands have implications for both ongoing and future planned observing programs that determine stellar mass and other physical properties of high-redshift galaxies solely via wide band photometry.

3

ČAVLOVIĆ, ANKA OZANA, and IVAN BEŠLIĆ. "APPLICATION OF PHOTOMETRY IN DETERMINING THE DUST MASS CONCENTRATION OF HARDWOODS." WOOD RESEARCH 66(4) 2021 66, no. 4 (September 9, 2021): 678–88. http://dx.doi.org/10.37763/wr.1336-4561/66.4.678688.

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Given the carcinogenicity of hardwood dust, the aim of this study was to determine the effectiveness of the photometric method for different types of woodworking machines and its application in determining the mass concentration of inhalable dust for raw and dry hardwoods. In addition to the optical part of the device, the input part of the measuring device contains the Institute of Occupational Medicine (IOM) inhalable dust filter holder. This correlation of gravimetric and photometric methods in determining the dust mass concentration showed that photometry underestimates the mass concentration measured gravimetrically. The results of this study recommend the application of a correction factor 2 for a timber band saw and a correction factor 3 for circular saws in determining the mass concentration of hardwood dust by the photometric method. It was showed that photometry can be used if the correction factor of the optical device has been previously tested for specific wood processing place.

4

Cernic, Vitor. "Stellar Population Photometric Synthesis with AI of S-PLUS galaxies." Proceedings of the International Astronomical Union 16, S362 (June 2020): 148–49. http://dx.doi.org/10.1017/s1743921322001430.

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AbstractWe trained a Neural Network that can obtain selected STARLIGHT parameters directly from S-PLUS photometry. The training set consisted of over 55 thousand galaxies with their stellar population parameters obtained from a STARLIGHT application by Cid Fernandes et al. (2005). These galaxies were crossmatched with the S-PLUS iDR 3 database, thus, recovering the photometry for the 12 band filters for 55803 objects. We also considered the spectroscopic redshift for each object which was obtained from the SDSS. Finally, we trained a fully connected Neural Network with the 12-band photometry + redshift as features, and targeted some of the STARLIGHT parameters, such as stellar mass and mean stellar age. The model performed very well for some parameters, for example, the stellar mass, with an error of 0.23 dex. In the future, we aim to apply the model to all S-PLUS galaxies, obtaining never-before-seen photometric synthesis for most objects in the catalogue.

5

Jerzykiewicz, M. "Two Aspects of Using Hipparcos Data for Studying Multiperiodic Stellar Pulsations." International Astronomical Union Colloquium 176 (2000): 46–49. http://dx.doi.org/10.1017/s0252921100057043.

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AbstractTwo aspects of using Hipparcos data for studying multiperiodic stellar pulsations involve (1) deriving frequencies of multiperiodic pulsators from Hipparcos Epoch Photometry, and (2) using Hipparcos parallaxes together with other data, such as the frequencies, frequency ratios and multicolor photometry, to identify pulsation modes. Details are examined by looking at the δ Scuti star DK Virginis. From Hipparcos Epoch Photometry, two frequencies are derived. These frequencies are then verified by showing that they also fit all available ground-based observations of the star. In addition, Hipparcos parallax and a photometric effective temperature are used to compare the position of DK Vir in the HR diagram with evolutionary tracks. The star turns out to be at the end of core-hydrogen-burning stage of its evolution or slightly beyond, with a mass of 2.2 M⊙, or somewhat smaller. The observed frequencies indicate that the two detected modes are p3 and p2, while the relatively large photometric amplitudes imply ℓ ≲ 2.

6

Schilbach, E., H. Meusinger, and J. Souchay. "Luminosity and Mass Functions for the Pleiades from the Schmidt Survey." Symposium - International Astronomical Union 164 (1995): 379. http://dx.doi.org/10.1017/s0074180900108976.

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From MAMA measurements of Tautenburg and OCA Schmidt plates we obtained proper motions and photographic UBVR photometry for ca. 45 000 stars up to B = 19 mag within a 17 square degree region in the Pleiades. An accuracy of 0.6 mag and 2 mas/year was estimated for magnitudes and proper motions, respectively. A sample of 554 cluster members was separated by use of both astrometric and photometric information on stars.

7

Schmehl, T., J. Gebhart, H. Schutte, A. Scharmann, and W. Seeger. "On-line laser-photometric monitoring of aerosol deposition in ventilated rabbit lungs." Journal of Applied Physiology 80, no. 1 (January 1, 1996): 351–56. http://dx.doi.org/10.1152/jappl.1996.80.1.351.

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A photometric technique was developed for on-line measurement of aerosol deposition in isolated, ventilated, and perfused rabbit lungs. A jet nebulizer was used for aerosolization of saline (hygroscopic particles) and di(2-ethylhexyl) sebacate (nonhygroscopic particles). Aerosol concentration (laser photometer, constructed for measurements in rabbit lungs) and flow rate (commercial pneumotachograph) were continuously monitored at the inlet of the tracheal cannula. Computer-assisted data processing allowed the breath-by-breath calculation of inhaled and exhaled aerosol mass, thus providing the deposition fraction. With the use of hygroscopic particles, however, this approach was hampered by the humidity-induced particle growth in the airways, leading to an overestimation of the aerosol concentration in exhaled air. This effect was corrected by an algorithm using a “particle growth factor” derived breath by breath from the photometer signal. To test the reliability of this approach, saline particles carrying technetium-99m label were aerosolized into rabbit lungs with the use of various ventilator settings, and the aerosol deposition was assessed in parallel by photometry and by radioactivity detection over the lung and over a trap in the exhaled-air circuit. Superimposable curves of cumulative aerosol deposition, with changes in kinetics dependent on the ventilator mode, were obtained. For a given ventilator setting, absolute values of the deposition fraction were 0.32 +/- 0.04 (radiotracer quantification) and 0.36 +/- 0.04 (photometry; means +/- SD; n = 4). We conclude that the presented laser-photometric technique allows reliable on-line monitoring of the deposition of both nonhygroscopic and hygroscopic aerosol particles in ventilated lungs.

8

Wu, Di, and Grzegorz Piszczek. "Standard protocol for mass photometry experiments." European Biophysics Journal 50, no. 3-4 (March 2, 2021): 403–9. http://dx.doi.org/10.1007/s00249-021-01513-9.

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9

Lombardo, Linda, Patrick François, Piercarlo Bonifacio, Elisabetta Caffau, Aroa del Mar Matas Pinto, Corinne Charbonnel, Georges Meynet, Lorenzo Monaco, Gabriele Cescutti, and Alessio Mucciarelli. "Young giants of intermediate mass." Astronomy & Astrophysics 656 (December 2021): A155. http://dx.doi.org/10.1051/0004-6361/202141408.

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Context. In the search of a sample of metal-poor bright giants using Strömgren photometry, we serendipitously found a sample of 26 young (ages younger than 1 Gyr) metal-rich giants, some of which have high rotational velocities. Aims. We determined the chemical composition and rotational velocities of these stars in order to compare them with predictions from stellar evolution models. These stars where of spectral type A to B when on the main sequence, and we therefore wished to compare their abundance pattern to that of main-sequence A and B stars. Methods. Stellar masses were derived by comparison of the position of the stars in the colour-magnitude diagram with theoretical evolutionary tracks. These masses, together with Gaia photometry and parallaxes, were used to derive the stellar parameters. We used spectrum synthesis and model atmospheres to determine chemical abundances for 16 elements (C, N, O, Mg, Al, Ca, Fe, Sr, Y, Ba, La, Ce, Pr, Nd, Sm, and Eu) and rotational velocities. Results. The age-metallicity degeneracy can affect photometric metallicity calibrations. We identify 15 stars as likely binary stars. All stars are in prograde motion around the Galactic centre and belong to the thin-disc population. All but one of the sample stars present low [C/Fe] and high [N/Fe] ratios together with constant [(C+N+O)/Fe], suggesting that they have undergone CNO processing and first dredge-up. The observed rotational velocities are in line with theoretical predictions of the evolution of rotating stars.

10

Innis, John, and Denis Coates. "NEW CMOS PHOTOMETRY AND ARCHIVAL PHOTOGRAPHIC OBSERVATIONS OF THE W UMA STAR V752 CEN: EXTENDING THE O-C RECORD OF PERIOD CHANGES." Open European Journal on Variable stars, no. 224 (2022): 1–18. http://dx.doi.org/10.5817/oejv2022-0224.

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We present new CMOS Bayer g-band photometry of the southern W UMa star V752 Cen, presenting two new times of primary minimum, and use archival photographic photometry from the Bamberg Sky Survey (mid 1960s) and the Harvard plate collection (∼1890 to 1990) to extend the O-C diagram back in time to ∼1900. Earlier authors have reported a constant period from the earliest published photometry in 1970 to about the year 2000, when a sudden change occurred to an increasing period. The archival photographic record presented here indicates the period was effectively constant back to 1900. Our 2020 data are also consistent with reported period increase. The V752 Cen system is known from earlier work to be a W UMa binary orbiting a lower mass spectroscopic binary. Our preliminary calculations, based on the reported centre-of-mass velocity change of the W UMa binary, suggest the wide orbit may have a period near 245 d, and could give rise to a light-travel time-effect of order 0.02 d. This does not however appear to be consistent with the SuperWASP photometric O-C results. Hence we suggest that considerable uncertainty exists concerning the properties of the wide orbit.

11

Fiorellino, Eleonora, Gabriella Zsidi, Ágnes Kóspál, Péter Ábrahám, Attila Bódi, Gaitee Hussain, Carlo F. Manara, and András Pál. "Accretion and Extinction Variations in the Low-mass Pre-main-sequence Binary System WX Cha*." Astrophysical Journal 938, no. 2 (October 1, 2022): 93. http://dx.doi.org/10.3847/1538-4357/ac912d.

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Abstract Light curves of young star systems show photometric variability due to different kinematic and physical processes. One of the main contributors to the photometric variability is the changing mass accretion rate, which regulates the interplay between the forming young star and the protoplanetary disk. We collected high-resolution spectroscopy in eight different epochs, as well as ground-based and space-borne multiepoch optical and infrared photometry of WX Cha, an M0 binary system, with an almost edge-on disk (i = 87°) in the Chamaeleon I star-forming region. Spectroscopic observations cover 72 days, the ground-based optical monitoring covers 42 days while space-borne TESS photometry extends for 56 days. The multiwavelength light curves exhibit quasi-periodic variability of 0.35–0.53 mag in the near-infrared, and of 1.3 mag in the g band. We studied the variability of selected emission lines that trace the accretion, computed the accretion luminosity and the mass accretion rate using empirical relations, and obtained values between L acc ∼ 1.6 L ⊙ − 3.2 L ⊙ and M ̇ acc ∼ 3.31 × 10 − 7 M ⊙ yr − 1 − 7.76 × 10 − 7 M ⊙ yr−1. Our results show that WX Cha is accreting at a rate larger than what is typical for T Tauri stars in the same star-forming region with the same stellar parameters. We theorize that this is due to the higher disk mass of WX Cha than what is usual for stars with similar stellar mass and to the binary nature of the system. Daily changes in the accretion luminosity and in the extinction can explain the photometric variability.

12

Kirby, Bennett C., Bryce A. Smith, and Brad N. Barlow. "Pulsational Velocity Variations of the Radial Mode sdBV Star BPM 36430." Research Notes of the AAS 7, no. 11 (November 30, 2023): 255. http://dx.doi.org/10.3847/2515-5172/ad1040.

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Abstract Hot subdwarf B stars are core-helium burning objects that were once red giants stripped of their outer H envelopes due to binary interactions. Many exhibit pulsations that can be used to determine fundamental stellar parameters like mass and radius. High-cadence TESS photometry of the sdB star BPM 36430 revealed it to be a hybrid-mode pulsator showing several g-mode pulsations and a single strong p-mode oscillation. The latter is likely a radial mode oscillation, given its period (342 s) and high photometric amplitude (2%). Using time-series spectroscopy from the Goodman spectrograph on the 4.1 m SOAR telescope, we detect a sinusoidal radial velocity variation with a semi-amplitude of 4.4 ± 0.4 km s−1 and period consistent with photometry of the p-mode oscillation. This detection provides further evidence the 342 s mode is radial in nature, and that the Baade–Wesselink method can be used with additional observations to constrain the stellar mass and radius.

13

Li, Yiwen, Weston B. Struwe, and Philipp Kukura. "Single molecule mass photometry of nucleic acids." Nucleic Acids Research 48, no. 17 (August 5, 2020): e97-e97. http://dx.doi.org/10.1093/nar/gkaa632.

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Abstract Mass photometry is a recently developed methodology capable of measuring the mass of individual proteins under solution conditions. Here, we show that this approach is equally applicable to nucleic acids, enabling their facile, rapid and accurate detection and quantification using sub-picomoles of sample. The ability to count individual molecules directly measures relative concentrations in complex mixtures without need for separation. Using a dsDNA ladder, we find a linear relationship between the number of bases per molecule and the associated imaging contrast for up to 1200 bp, enabling us to quantify dsDNA length with up to 2 bp accuracy. These results introduce mass photometry as an accurate, rapid and label-free single molecule method complementary to existing DNA characterization techniques.

14

Roquette, Julia, Jerome Bouvier, Estelle Moraux, Herve Bouy, Jonathan Irwin, Suzanne Aigrain, and Régis Lachaume. "The rotation of low mass stars at 30 Myr in the cluster NGC 3766." Proceedings of the International Astronomical Union 15, S354 (June 2019): 200–203. http://dx.doi.org/10.1017/s1743921319009797.

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AbstractTogether with the stellar rotation, the spotted surfaces of low-mass magnetically active stars produce modulations in their brightness. These modulations can be resolved by photometric variability surveys, allowing direct measurements of stellar spin rates. In this proceedings, we present results of a multisite photometric survey dedicated to the measurement of spin rates in the 30 Myr cluster NGC 3766. Inside the framework of the Monitor Project, the cluster was monitored during 2014 in the i-band by the Wide Field Imager at the MPG/ESO 2.2-m telescope. Data from Gaia-DR2 and grizY photometry from DECam/CTIO were used to identify cluster members. We present spin rates measured for ⁓200 cluster members.

15

Zhang, X. B. "The eclipsing binary IU Per and its intrinsic oscillations." Proceedings of the International Astronomical Union 4, S252 (April 2008): 429–30. http://dx.doi.org/10.1017/s1743921308023417.

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AbstractThe results of a long-term time-series photometry of the short-period eclipsing binary IU Per are reported. The observation confirms the intrinsic δ Scuti-like pulsation of the star as discovered by previous authors. A photometric solution for the binary system was carried out with the new data. Based on which, the pure oscillation light variations from the mass-accreting primary component were extracted. A Fourier analysis reveals four pulsation modes. Combining with the photometric solution, a preliminary mode identification was given.

16

Li, Yang A., Luis C. Ho, Jinyi Shangguan, Ming-Yang Zhuang, and Ruancun Li. "Panchromatic Photometry of Low-redshift, Massive Galaxies Selected from SDSS Stripe 82." Astrophysical Journal Supplement Series 267, no. 1 (July 1, 2023): 17. http://dx.doi.org/10.3847/1538-4365/acd4b5.

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Abstract The broadband spectral energy distribution of a galaxy encodes valuable information on its stellar mass, star formation rate (SFR), dust content, and possible fractional energy contribution from nonstellar sources. We present a comprehensive catalog of panchromatic photometry, covering 17 bands from the far-ultraviolet to 500 μm, for 2685 low-redshift (z = 0.01–0.11), massive (M * > 1010 M ⊙) galaxies selected from the Stripe 82 region of the Sloan Digital Sky Survey, one of the largest areas with relatively deep, uniform observations over a wide range of wavelengths. Taking advantage of the deep optical coadded images, we develop a hybrid approach for matched-aperture photometry of the multiband data. We derive robust uncertainties and upper limits for undetected galaxies, deblend interacting/merging galaxies and sources in crowded regions, and treat contamination by foreground stars. We perform spectral energy distribution fitting to derive the stellar mass, SFR, and dust mass, critically assessing the influence of flux upper limits for undetected photometric bands and applying corrections for systematic uncertainties based on extensive mock tests. Comparison of our measurements with those of commonly used published catalogs reveals good agreement for the stellar masses. While the SFRs of galaxies on the star-forming main sequence show reasonable consistency, galaxies in and below the green valley show considerable disagreement between different sets of measurements. Our analysis suggests that one should incorporate the most accurate and inclusive photometry into the spectral energy distribution analysis, and that care should be exercised in interpreting the SFRs of galaxies with moderate to weak star formation activity.

17

Loup, Cécile, Mark Allen, Ariane Lançon, and Anais Oberto. "OH/IR stars versus YSOs in infrared photometric surveys." Proceedings of the International Astronomical Union 14, S343 (August 2018): 454–55. http://dx.doi.org/10.1017/s1743921318007901.

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AbstractAGB stars play a major role in the chemical evolution of the galaxies. It thus is important to establish reliable photometric selection criteria to count them, especially AGB stars at the last stages of AGB evolution like OH/IR stars. Here, we have identified about 1500 OH/IR stars and 500 YSOs with methanol masers, in all major mid– and far–infrared surveys (IRAS, MSX, AKARI, WISE, GLIMPSE, and Hi–Gal). We show that AGB stars with high mass-loss rates cannot be disentagled from YSOs with only mid–infrared photometry; far–infrared photometry is essential. In the region observed by GLIMPSE, we show that the proportion of AGB stars has been severely underestimated in previous works: about 70% of “intrinsically” red objects in GLIMPSE are AGB stars rather than YSOs.

18

Helton, Jakob M., Fengwu Sun, Charity Woodrum, Kevin N. Hainline, Christopher N. A. Willmer, George H. Rieke, Marcia J. Rieke, et al. "The JWST Advanced Deep Extragalactic Survey: Discovery of an Extreme Galaxy Overdensity at z = 5.4 with JWST/NIRCam in GOODS-S." Astrophysical Journal 962, no. 2 (February 1, 2024): 124. http://dx.doi.org/10.3847/1538-4357/ad0da7.

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Abstract We report the discovery of an extreme galaxy overdensity at z = 5.4 in the GOODS-S field using James Webb Space Telescope (JWST)/NIRCam imaging from JADES and JEMS alongside JWST/NIRCam wide-field slitless spectroscopy from FRESCO. We identified potential members of the overdensity using Hubble Space Telescope+JWST photometry spanning λ = 0.4–5.0 μm. These data provide accurate and well-constrained photometric redshifts down to m ≈ 29–30 mag. We subsequently confirmed N = 81 galaxies at 5.2 < z < 5.5 using JWST slitless spectroscopy over λ = 3.9–5.0 μm through a targeted line search for Hα around the best-fit photometric redshift. We verified that N = 42 of these galaxies reside in the field, while N = 39 galaxies reside in a density around ∼10 times that of a random volume. Stellar populations for these galaxies were inferred from the photometry and used to construct the star-forming main sequence, where protocluster members appeared more massive and exhibited earlier star formation (and thus older stellar populations) when compared to their field galaxy counterparts. We estimate the total halo mass of this large-scale structure to be 12.6 ≲ log 10 M halo / M ⊙ ≲ 12.8 using an empirical stellar mass to halo mass relation, which is likely an underestimate as a result of incompleteness. Our discovery demonstrates the power of JWST at constraining dark matter halo assembly and galaxy formation at very early cosmic times.

19

Nikolic, Goran, Milorad Cakic, and Ljubomir Ilic. "Specific refractive index increments of inulin." Journal of the Serbian Chemical Society 66, no. 6 (2001): 397–401. http://dx.doi.org/10.2298/jsc0106397n.

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The specific refractive index increments (dn/dc) of inulin in water, at 25 ?C, were measured at different wavelengths (436, 546 and 589 nm) using a BP-differential refractometer. The dn/dc at the operating wavelength (633 nm) of the laser light scattering photometer was calculated by an approximate method. This value can be used to determine the absolute molar mass and the second virial coefficient of inulin by light scattering photometry.

20

Sohn, Jubee, Margaret J. Geller, Ho Seong Hwang, Daniel G. Fabricant, Yousuke Utsumi, and Ivana Damjanov. "HectoMAP: The Complete Redshift Survey (Data Release 2)." Astrophysical Journal 945, no. 2 (March 1, 2023): 94. http://dx.doi.org/10.3847/1538-4357/acb925.

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Abstract HectoMAP is a dense redshift survey of 95,403 galaxies based primarily on MMT spectroscopy with a median redshift z = 0.345. The survey covers 54.64 deg2 in a 1.°5 wide strip across the northern sky centered at a decl. of 43.°25. We report the redshift, the spectral indicator D n 4000, and the stellar mass. The red-selected survey is 81% complete for 55,962 galaxies with (g − r) > 1 and r < 20.5; it is 72% complete for 32,908 galaxies with (g − r) > 1, (r − i) > 0.5 and 20.5 < r < 21.3. Comparison of the survey basis SDSS photometry with the HSC-SSP photometry demonstrates that HectoMAP provides complete magnitude-limited surveys based on either photometric system. We update the comparison between the HSC-SSP photometric redshifts with HectoMAP spectroscopic redshifts; the comparison demonstrates that the HSC-SSP photometric redshifts have improved between the second and third data releases. HectoMAP is a foundation for examining the quiescent galaxy population (63% of the survey), clusters of galaxies, and the cosmic web. HectoMAP is completely covered by the HSC-SSP survey, thus enabling a variety of strong- and weak-lensing investigations.

21

Wagner, Christina, Felix F. Fuchsberger, Bernd Innthaler, Robert Pachlinger, Irene Schrenk, Martin Lemmerer, and Ruth Birner-Gruenberger. "Automated Mass Photometry of Adeno-Associated Virus Vectors from Crude Cell Extracts." International Journal of Molecular Sciences 25, no. 2 (January 9, 2024): 838. http://dx.doi.org/10.3390/ijms25020838.

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Mass photometry (MP) is a fast and simple analysis method for the determination of the proportions of subpopulations in an AAV sample. It is label-free and requires minimal sample volumes between 5–10 µL, which makes it a promising candidate over orthogonal techniques such as analytical ultracentrifugation (AUC), cryo-transmission electron microscopy (Cryo-TEM) or charge-detection mass spectrometry (CDMS). However, these methods are limited in their application to purified samples only. Here we developed a purification step based on single-domain monospecific antibody fragments immobilised on either a poly(styrene-divinylbenzene) resin or on magnetic beads prior to MP analysis that allows the quantification of empty, partially filled, full and overfull AAV vectors in crude cell extracts. This is aimed at identifying potentially promising harvest conditions that yield large numbers of filled AAV vectors during the early stages of the viral vector development platform, e.g., the type of transfection reagent used. Furthermore, we provide a direct comparison of the automated and manual handling of the mass photometer with respect to the quantities of AAV subspecies, molar mass of the capsid and payload, and highlight the differences between the “buffer-free” sample measurement and the “buffer-dilution” mode. In addition, we provide information on which candidates to use for calibration and demonstrate the limitations of the mass photometer with respect to the estimation of the capsid titer.

22

Bilicki, M., A. Dvornik, H. Hoekstra, A. H. Wright, N. E. Chisari, M. Vakili, M. Asgari, et al. "Bright galaxy sample in the Kilo-Degree Survey Data Release 4." Astronomy & Astrophysics 653 (September 2021): A82. http://dx.doi.org/10.1051/0004-6361/202140352.

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We present a bright galaxy sample with accurate and precise photometric redshifts (photo-zs), selected using ugriZYJHKs photometry from the Kilo-Degree Survey (KiDS) Data Release 4. The highly pure and complete dataset is flux-limited at r < 20 mag, covers ∼1000 deg2, and contains about 1 million galaxies after artifact masking. We exploit the overlap with Galaxy And Mass Assembly spectroscopy as calibration to determine photo-zs with the supervised machine learning neural network algorithm implemented in the ANNz2 software. The photo-zs have a mean error of |⟨δz⟩|∼5 × 10−4 and low scatter (scaled mean absolute deviation of ∼0.018(1 + z)); they are both practically independent of the r-band magnitude and photo-z at 0.05 < zphot < 0.5. Combined with the 9-band photometry, these allow us to estimate robust absolute magnitudes and stellar masses for the full sample. As a demonstration of the usefulness of these data, we split the dataset into red and blue galaxies, used them as lenses, and measured the weak gravitational lensing signal around them for five stellar mass bins. We fit a halo model to these high-precision measurements to constrain the stellar-mass–halo-mass relations for blue and red galaxies. We find that for high stellar mass (M⋆ > 5 × 1011 M⊙), the red galaxies occupy dark matter halos that are much more massive than those occupied by blue galaxies with the same stellar mass.

23

Duey, Francis, James Schombert, Stacy McGaugh, and Federico Lelli. "The Baryonic Tully–Fisher Relation. I. WISE/Spitzer Photometry." Astronomical Journal 168, no. 1 (June 20, 2024): 19. http://dx.doi.org/10.3847/1538-3881/ad454c.

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Abstract We present Wide-field Infrared Survey Explorer (WISE) W1 photometry of the Spitzer Photometry and Accurate Rotation Curves sample. The baseline of near-IR fluxes is established for use by stellar mass models, a key component to the baryonic Tully–Fisher relation and other kinematic galaxies scaling relations. We focus this paper on determination of the characteristics of the W1 fluxes compared to IRAC 3.6 μm fluxes, internal accuracy limitations from photometric techniques, external accuracy by comparison to other work in the literature and the range of W1 to IRAC 3.6 μm colors. We outline the behavior of SDSS g, W1 and IRAC 3.6 colors with respect to underlying spectral energy distribution features. We also note a previously unknown correlation between WISE colors and the central surface brightness, probably related to the low metallicity of low-surface-brightness dwarfs.

24

Holmbo, S., M. D. Stritzinger, B. J. Shappee, M. A. Tucker, W. Zheng, C. Ashall, M. M. Phillips, et al. "Discovery and progenitor constraints on the Type Ia supernova 2013gy." Astronomy & Astrophysics 627 (July 2019): A174. http://dx.doi.org/10.1051/0004-6361/201834389.

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We present an early-phase g-band light curve and visual-wavelength spectra of the normal Type Ia supernova (SN) 2013gy. The light curve is constructed by determining the appropriate S-corrections to transform KAIT natural-system B- and V-band photometry and Carnegie Supernova Project natural-system g-band photometry to the Pan-STARRS1 g-band natural photometric system. A Markov chain Monte Carlo calculation provides a best-fit single power-law function to the first ten epochs of photometry described by an exponent of 2.16+0.06−0.06 and a time of first light of MJD 56629.4+0.1−0.1, which is 1.93+0.12−0.13 days (i.e., < 48 h) before the discovery date (2013 December 4.84 UT) and −19.10+0.12−0.13 days before the time of B-band maximum (MJD 56648.5 ± 0.1). The estimate of the time of first light is consistent with the explosion time inferred from the evolution of the Si IIλ6355 Doppler velocity. Furthermore, discovery photometry and previous nondetection limits enable us to constrain the companion radius down to Rc ≤ 4 R⊙. In addition to our early-time constraints, we used a deep +235 day nebular-phase spectrum from Magellan/IMACS to place a stripped H-mass limit of < 0.018 M⊙. Combined, these limits effectively rule out H-rich nondegenerate companions.

25

Apellániz, J. Maíz. "The range of validity of cluster masses and ages derived from broad-band photometry." Proceedings of the International Astronomical Union 5, S266 (August 2009): 100–105. http://dx.doi.org/10.1017/s1743921309990937.

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AbstractI analyze the stochastic effects introduced by sampling the stellar initial mass function (SIMF) in the derivation of the individual masses and the cluster mass function (CMF) from broad-band visible/near-infrared unresolved photometry. The classical method of using unweighted U BV photometry to simultaneously establish ages and extinctions of stellar clusters is found to be unreliable for clusters older than ≈30 Myr, even for relatively large cluster masses. On the other hand, augmenting the filter set to include longer-wavelength filters and using weights for each filter increases the range of masses and ages that can be measured accurately with unresolved photometry. Nevertheless, a relatively large range of masses and ages is found to be dominated by SIMF sampling effects that render the observed masses useless, even when using U BV RI JHK photometry.

26

Asor, Roi, and Philipp Kukura. "Characterising biomolecular interactions and dynamics with mass photometry." Current Opinion in Chemical Biology 68 (June 2022): 102132. http://dx.doi.org/10.1016/j.cbpa.2022.102132.

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27

Pfitzner, Emanuel, Daniel Cole, and Philipp Kukura. "Combination of single-molecule fluorescence and mass photometry." Biophysical Journal 121, no. 3 (February 2022): 430a—431a. http://dx.doi.org/10.1016/j.bpj.2021.11.611.

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28

Lupton, R. H., and J. E. Gunn. "M13 - Main sequence photometry and the mass function." Astronomical Journal 91 (February 1986): 317. http://dx.doi.org/10.1086/114012.

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29

Hodgkin, S. T., D. J. Pinfield, R. F. Jameson, I. A. Steele, M. R. Cossburn, and N. C. Hambly. "Infrared photometry of low-mass stars in Praesepe." Monthly Notices of the Royal Astronomical Society 310, no. 1 (November 21, 1999): 87–96. http://dx.doi.org/10.1046/j.1365-8711.1999.02929.x.

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30

Graciani, Guillaume, and Tae-Young Yoon. "The New Kid on the Block: Mass Photometry." Molecules and Cells 46, no. 3 (March 31, 2023): 187–89. http://dx.doi.org/10.14348/molcells.2023.0017.

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31

Elmhamdi, A., N. N. Chugai та I. J. Danziger. "56Ni Mass in Type IIP SNe: Light Curves and Hα Luminosity Diagnostics". International Astronomical Union Colloquium 192 (2005): 303–8. http://dx.doi.org/10.1017/s0252921100009337.

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SummaryWe analyze late-time observations, available photometry and spectra, of a sample of type II plateau supernovae (SNe IIP). The possibility of using Hα luminosity at the nebular epoch as a tracer of 56Ni mass in this class of objects is investigated, yielding a consistency with the photometry-based estimates within 20%. Interesting correlations are found and their impacts on our present understanding of the physics of core collapse SNe are discussed.

32

Seidensticker, K. J., and Th Schmidt-Kaler. "Extinction Maps of Dust Clouds from Surface Photometry." Symposium - International Astronomical Union 139 (1990): 239–40. http://dx.doi.org/10.1017/s0074180900240795.

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We present a new method, based on surface photometry, which allows one to make the spatial resolution of extinction maps of dark clouds as fine as necessary. Applying this technique to the Coalsack (l = 302°, b = 0°), we derived an extinction map and the dust mass MD = (62 ± 25) M⊙. The density was found to vary ρ ~ r−0.8, typical for stable clouds.

33

Nikiforova, A. A., P. V. Baklanov, S. I. Blinnikov, D. A. Blinov, T. S. Grishina, Yu V. Troitskaya, D. A. Morozova, E. N. Kopatskaya, E. G. Larionova, and I. S. Troitsky. "Parameters of the type-IIP supernova SN 2012aw." Monthly Notices of the Royal Astronomical Society 504, no. 3 (April 19, 2021): 3544–49. http://dx.doi.org/10.1093/mnras/stab1093.

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ABSTRACT We present the results the photometric observations of the Type IIP supernova SN 2012aw obtained for the time interval from 7 to 371 d after the explosion. Using the previously published values of the photospheric velocities, we have computed the hydrodynamic model which simultaneously reproduced the photometry observations and velocity measurements. We found the parameters of the pre-supernova: radius R = 500 R⊙, nickel mass M(56Ni$)\, \sim 0.06\, \rm M_\odot$, pre-supernova mass 25 M⊙, mass of ejected envelope 23.6 M⊙, explosion energy E ∼ 2 × 1051 erg. The model progenitor mass M = 25 M⊙ significantly exceeds the upper limit mass M = 17 M⊙, obtained from analysis the pre-SNe observations. This result confirms once more that the ’Red Supergiant Problem’ must be resolved by stellar evolution and supernova explosion theories in interaction with observations.

34

Lendl, Monika, François Bouchy, Samuel Gill, Louise D. Nielsen, Oliver Turner, Keivan Stassun, Jack S. Acton, et al. "TOI-222: a single-transit TESS candidate revealed to be a 34-d eclipsing binary with CORALIE, EulerCam, and NGTS." Monthly Notices of the Royal Astronomical Society 492, no. 2 (December 23, 2019): 1761–69. http://dx.doi.org/10.1093/mnras/stz3545.

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ABSTRACT We report the period, eccentricity, and mass determination for the Transiting Exoplanet Survey Satellite (TESS) single-transit event candidate TOI-222, which displayed a single 3000 ppm transit in the TESS 2-min cadence data from Sector 2. We determine the orbital period via radial velocity measurements (P = 33.9 d), which allowed for ground-based photometric detection of two subsequent transits. Our data show that the companion to TOI-222 is a low-mass star, with a radius of $0.18_{-0.10}^{+0.39}$ R⊙ and a mass of 0.23 ± 0.01 M⊙. This discovery showcases the ability to efficiently discover long-period systems from TESS single-transit events using a combination of radial velocity monitoring coupled with high-precision ground-based photometry.

35

Ragosta, Fabio, Marcella Marconi, Roberto Molinaro, Vincenzo Ripepi, Maria Rosa L. Cioni, Maria Ida Moretti, Martin A. T. Groenewegen, et al. "The VMC survey – XXXV. model fitting of LMC Cepheid light curves." Monthly Notices of the Royal Astronomical Society 490, no. 4 (October 14, 2019): 4975–84. http://dx.doi.org/10.1093/mnras/stz2881.

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ABSTRACT We present the results of the light curve model fitting technique applied to optical and near-infrared photometric data for a sample of 18 Classical Cepheids (11 fundamentals and 7 first overtones) in the Large Magellanic Cloud (LMC). We use optical photometry from the OGLE III data base and near-infrared photometry obtained by the European Southern Observatory public survey ‘VISTA near-infrared survey of the Magellanic Clouds system’. Iso-periodic non-linear convective model sequences have been computed for each selected Cepheid in order to reproduce the multifilter light-curve amplitudes and shape details. The inferred individual distances provide an intrinsic weighted mean value for the LMC distance modulus of μ0 = 18.56 mag with a standard deviation of 0.13 mag. We derive also the Period–Radius, the Period–Luminosity, and the Period–Wesenheit relations that are consistent with similar relations in the literature. The intrinsic masses and luminosities of the best-fitting models show that all the investigated pulsators are brighter than the predictions of the canonical evolutionary mass–luminosity relation, suggesting a significant efficiency of non-canonical phenomena, such as overshooting, mass-loss, and/or rotation.

36

Song, Jie, GuanWen Fang, Zesen Lin, Yizhou Gu, and Xu Kong. "Solution to the Conflict between the Estimations of Resolved and Unresolved Galaxy Stellar Mass from the Perspective of JWST." Astrophysical Journal 958, no. 1 (November 1, 2023): 82. http://dx.doi.org/10.3847/1538-4357/ad0365.

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Abstract By utilizing the spatially resolved photometry of galaxies at 0.2 < z < 3.0 in the CEERS field, we estimate the resolved and unresolved stellar mass via fitting of the spectral energy distribution (SED) to study the discrepancy between them. We first compare M * derived from photometry with and without the JWST wavelength coverage and find that M * can be overestimated by up to 0.2 dex when lacking rest-frame near-infrared (NIR) data. The SED fitting process tends to overestimate both stellar age and dust attenuation in the absence of rest-frame NIR data, consequently leading to a larger observed mass-to-light ratio and hence an elevated M *. With the inclusion of the JWST NIR photometry, we find no significant disparity between the estimates of resolved and unresolved stellar mass, providing a plausible solution to the conflict between them out to z ∼ 3. Further investigation demonstrates that reliable M * estimates can be obtained, regardless of whether they are derived from spatially resolved or spatially unresolved photometry, so long as the reddest filter included in the SED fitting has a rest-frame wavelength longer than 10000 Å.

37

Wang, Xin. "Revisiting Abell 2744: a powerful synergy of GLASS spectroscopy and HFF photometry." Proceedings of the International Astronomical Union 11, A29B (August 2015): 776–78. http://dx.doi.org/10.1017/s1743921316006785.

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AbstractWe present new emission line identifications and improve the lensing reconstruction of the mass distribution of galaxy cluster Abell 2744 using the Grism Lens-Amplified Survey from Space (GLASS) spectroscopy and the Hubble Frontier Fields (HFF) imaging. We performed blind and targeted searches for faint line emitters on all objects, including the arc sample, within the field of view (FoV) of GLASS prime pointings. We report 55 high quality spectroscopic redshifts, 5 of which are for arc images. We also present an extensive analysis based on the HFF photometry, measuring the colors and photometric redshifts of all objects within the FoV, and comparing the spectroscopic and photometric redshift estimates. In order to improve the lens model of Abell 2744, we develop a rigorous algorithm to screen arc images, based on their colors and morphology, and selecting the most reliable ones to use. As a result, 25 systems (corresponding to 72 images) pass the screening process and are used to reconstruct the gravitational potential of the cluster pixellated on an adaptive mesh. The resulting total mass distribution is compared with a stellar mass map obtained from the Spitzer Frontier Fields data in order to study the relative distribution of stars and dark matter in the cluster.

38

Koçak, D., T. İçli, and K. Yakut. "Multicolour photometry of SS 433." Proceedings of the International Astronomical Union 14, S346 (August 2018): 252–54. http://dx.doi.org/10.1017/s1743921318008529.

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AbstractWe presented long-term optical observations of the high mass X-ray binary system SS 433 (V1343 Aql) with a black hole component. New observations have been obtained by using the 0.6m telescope at the TÜBİTAK National Observatory (TUG) in B, V, R and I filters. We aim to investigate the long-term photometric behavior of the system.

39

Charles, P. A. "Black-Hole Systems: Optical Spectroscopy and IR Photometry." Symposium - International Astronomical Union 165 (1996): 341–50. http://dx.doi.org/10.1017/s0074180900055807.

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The X-ray transient systems have provided the first opportunities for detailed studies of the mass losing star in low-mass X-ray binaries. During X-ray quiescence the cool star is the dominant light source in the red and near-IR. Optical spectroscopy yields the mass function (itself a lower limit to the compact-object mass), the rotational broadening leads to the mass ratio, q (assuming only that the star fills its Roche lobe), and the IR ellipsoidal light curve gives the system inclination (for high q). In such cases, a complete solution to the system parameters is possible, and this has been performed for A 0620-00 (V616 Mon) and GS 2023+338 (V404 Cyg), leading to the first accurate black-hole masses (which are in the range 10–12 M⊙).

40

Biller, B. A., A. Grandjean, S. Messina, S. Desidera, P. Delorme, A. M. Lagrange, F. J. Hambsch, et al. "Dynamical masses for two M1 + mid-M dwarf binaries monitored during the SPHERE-SHINE survey." Astronomy & Astrophysics 658 (February 2022): A145. http://dx.doi.org/10.1051/0004-6361/202142438.

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We present orbital fits and dynamical masses for HIP 113201AB and HIP 36985AB, two M1 + mid-M dwarf binary systems monitored as part of the SPHERE-SHINE survey. To robustly determine the age of both systems via gyrochronology, we undertook a photometric monitoring campaign for HIP 113201 and GJ 282AB, the two wide K star companions to HIP 36985, using the 40 cm Remote Observatory Atacama Desert telescope. Based on this monitoring and gyrochronological relationships, we adopt ages of 1.2 ± 0.1 Gyr for HIP 113201AB and 750 ± 100 Myr for HIP 36985AB. These systems are sufficiently old that we expect that all components of these binaries have reached the main sequence. To derive dynamical masses for all components of the HIP 113201AB and HIP 36985AB systems, we used parallel-tempering Markov chain Monte Carlo sampling to fit a combination of radial velocity, direct imaging, and Gaia and HIPPARCOS astrometry. Fitting the direct imaging and radial velocity data for HIP 113201 yields a primary mass of 0.54 ± 0.03 M⊙, fully consistent with its M1 spectral type, and a secondary mass of 0.145 ± M⊙. The secondary masses derived with and without including HIPPARCOS-Gaia data are all considerably more massive than the 0.1 M⊙ mass estimated from the photometry of the companion. Thus, the dynamical impacts of this companion suggest that it is more massive than expected from its photometry. An undetected brown dwarf companion to HIP 113201B could be a natural explanation for this apparent discrepancy. At an age >1 Gyr, a 30 MJup companion to HIP 113201B would make a negligible (<1%) contribution to the system luminosity but could have strong dynamical impacts. Fitting the direct imaging, radial velocity, and HIPPARCOS-Gaia proper motion anomaly for HIP 36985AB, we find a primary mass of 0.54 ± 0.01 M⊙ and a secondary mass of 0.185 ± 0.001 M⊙, which agree well with photometric estimates of component masses, the masses estimated from MK– mass relationships for M dwarf stars, and previous dynamical masses in the literature.

41

Hobson, Melissa J., Trifon Trifonov, Thomas Henning, Andrés Jordán, Felipe Rojas, Nestor Espinoza, Rafael Brahm, et al. "TOI-199 b: A Well-characterized 100 day Transiting Warm Giant Planet with TTVs Seen from Antarctica." Astronomical Journal 166, no. 5 (October 18, 2023): 201. http://dx.doi.org/10.3847/1538-3881/acfc1d.

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Abstract We present the spectroscopic confirmation and precise mass measurement of the warm giant planet TOI-199 b. This planet was first identified in TESS photometry and confirmed using ground-based photometry from ASTEP in Antarctica including a full 6.5 hr long transit, PEST, Hazelwood, and LCO; space photometry from NEOSSat; and radial velocities (RVs) from FEROS, HARPS, CORALIE, and CHIRON. Orbiting a late G-type star, TOI-199 b has a 104.854 − 0.002 + 0.001 day period, a mass of 0.17 ± 0.02 M J, and a radius of 0.810 ± 0.005 R J. It is the first warm exo-Saturn with a precisely determined mass and radius. The TESS and ASTEP transits show strong transit timing variations (TTVs), pointing to the existence of a second planet in the system. The joint analysis of the RVs and TTVs provides a unique solution for the nontransiting companion TOI-199 c, which has a period of 273.69 − 0.22 + 0.26 days and an estimated mass of 0.28 − 0.01 + 0.02 M J . This period places it within the conservative habitable zone.

42

Adams, N. J., R. A. A. Bowler, M. J. Jarvis, B. Häußler, and C. D. P. Lagos. "Evolution of the galaxy stellar mass function: evidence for an increasing M* from z = 2 to the present day." Monthly Notices of the Royal Astronomical Society 506, no. 4 (July 15, 2021): 4933–51. http://dx.doi.org/10.1093/mnras/stab1956.

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ABSTRACT Utilizing optical and near-infrared broad-band photometry covering >5 deg2 in two of the most well-studied extragalactic legacy fields (COSMOS and XMM-LSS), we measure the galaxy stellar mass function (GSMF) between 0.1 < z < 2.0. We explore in detail the effect of two source extraction methods (SExtractor and ProFound) in addition to the inclusion/exclusion of Spitzer IRAC 3.6 and 4.5 μm photometry when measuring the GSMF. We find that including IRAC data reduces the number of massive (log10(M/M⊙) > 11.25) galaxies found due to improved photometric redshift accuracy, but has little effect on the more numerous lower-mass galaxies. We fit the resultant GSMFs with double Schechter functions down to log10(M/M⊙) = 7.75 (9.75) at z = 0.1 (2.0) and find that the choice of source extraction software has no significant effect on the derived best-fitting parameters. However, the choice of methodology used to correct for the Eddington bias has a larger impact on the high-mass end of the GSMF, which can partly explain the spread in derived M* values from previous studies. Using an empirical correction to model the intrinsic GSMF, we find evidence for an evolving characteristic stellar mass with δlog10(M*/M⊙)/δz = $-0.16\pm 0.05 \, (-0.11\pm 0.05)$, when using SExtractor (ProFound). We argue that with widely quenched star formation rates in massive galaxies at low redshift (z < 0.5), additional growth via mergers is required in order to sustain such an evolution to a higher characteristic mass.

43

Scott Gaudi, B. "Microlensing Constraints on Low-Mass Companions." Symposium - International Astronomical Union 211 (2003): 305–8. http://dx.doi.org/10.1017/s0074180900210826.

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Microlensing is sensitive to binary, brown dwarf (BD), and planetary companions to normal stars in the Galactic bulge with separations between about 1–10 AU. The accurate, densely-sampled photometry of microlensing events needed to detect planetary companions has been achieved by several follow-up collaborations. Detailed analysis of microlensing events toward the bulge demonstrates that less than 45% of M-dwarfs in the bulge have MJup companions between 1 and 5 AU. Detection of binary and BD companions using microlensing is considerably easier; however, the interpretation is hampered by their non-perturbative influence on the parent lightcurve. I demonstrate that ~ 25% of BD companions with separations 1 – 10AU should be detectable with survey-quality data (~ 1 day sampling and ~ 5% photometry). Survey data is more amenable to generic, brute-force analysis methods and less prone to selection biases. An analysis of the ~ 1500 microlensing events detected by OGLE-III in the next three years should test whether the BD desert exists at separations 1 – 10AU from M-dwarfs in the Galactic bulge.

44

Ksoll, Victor F., Lynton Ardizzone, Ralf Klessen, Ullrich Koethe, Elena Sabbi, Massimo Robberto, Dimitrios Gouliermis, Carsten Rother, Peter Zeidler, and Mario Gennaro. "Stellar parameter determination from photometry using invertible neural networks." Monthly Notices of the Royal Astronomical Society 499, no. 4 (November 5, 2020): 5447–85. http://dx.doi.org/10.1093/mnras/staa2931.

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ABSTRACT Photometric surveys with the Hubble Space Telescope (HST) allow us to study stellar populations with high-resolution and deep coverage, with estimates of the physical parameters of the constituent stars being typically obtained by comparing the survey data with adequate stellar evolutionary models. This is a highly non-trivial task due to effects such as differential extinction, photometric errors, low filter coverage, or uncertainties in the stellar evolution calculations. These introduce degeneracies that are difficult to detect and break. To improve this situation, we introduce a novel deep learning approach, called conditional invertible neural network (cINN), to solve the inverse problem of predicting physical parameters from photometry on an individual star basis and to obtain the full posterior distributions. We build a carefully curated synthetic training data set derived from the PARSEC stellar evolution models to predict stellar age, initial/current mass, luminosity, effective temperature, and surface gravity. We perform tests on synthetic data from the MIST and Dartmouth models, and benchmark our approach on HST data of two well-studied stellar clusters, Westerlund 2 and NGC 6397. For the synthetic data, we find overall excellent performance, and note that age is the most difficult parameter to constrain. For the benchmark clusters, we retrieve reasonable results and confirm previous findings for Westerlund 2 on cluster age ($1.04_{-0.90}^{+8.48}\, \mathrm{Myr}$), mass segregation, and the stellar initial mass function. For NGC 6397, we recover plausible estimates for masses, luminosities, and temperatures, however, discrepancies between stellar evolution models and observations prevent an acceptable recovery of age for old stars.

45

Jahreiß, Hartmut, and Wilhelm Gliese. "The Third Catalogue of Nearby Stars — Results and Conclusions." Symposium - International Astronomical Union 156 (1993): 107–12. http://dx.doi.org/10.1017/s0074180900173024.

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The nearby stars constitute the statistically most complete and therefore most representative sample of stars in our Galaxy. Only this sample allows a direct investigation of luminosity function and kinematics of low-mass stars.A study of the Third Catalogue of Nearby Stars reveals a considerable increase — not only in quantity but also in quality — in our knowledge of the immediate solar neighbourhood, and reflects very nicely the progress achieved during the last decades — especially in astrometry and photometry. Expectations for the near future (HIPPARCOS) and desiderata for further astrometric and photometric work will be discussed.

46

Zaidi, Kumail, Danilo Marchesini, Casey Papovich, Jacqueline Antwi-Danso, Mario Nonino, Marianna Annunziatella, Gabriel Brammer, et al. "The FENIKS Survey: Multiwavelength Photometric Catalog in the UDS Field, and Catalogs of Photometric Redshifts and Stellar Population Properties." Astrophysical Journal 969, no. 2 (July 1, 2024): 84. http://dx.doi.org/10.3847/1538-4357/ad45fa.

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Abstract We present the construction of a deep multiwavelength point-spread-function-matched photometric catalog in the Ultra-Deep Survey (UDS) field following the final UKIDSS UDS release. The catalog includes photometry in 24 filters, from the MegaCam-uS 0.38 μm band to the Spitzer-IRAC 8 μm band, over ∼0.9 deg2 and with a 5σ depth of 25.3 AB in the K-band detection image. The catalog, containing ≈188,564 (136,235) galaxies at 0.2 < z < 8.0 with stellar mass log ( M * / M ⊙ ) > 8 and K-band total magnitude K < 25.2 (24.3) AB, enables a range of extragalactic studies. We also provide photometric redshifts, corresponding redshift probability distributions, and rest-frame absolute magnitudes and colors derived using the template-fitting code eazy-py. Photometric redshift errors are less than 3%−4% at z < 4 across the full brightness range in the K band and stellar mass range 8 < log ( M * / M ⊙ ) < 12 . Stellar population properties (e.g., stellar mass, star formation rate, dust extinction) are derived from the modeling of the spectral energy distributions using the codes FAST and Dense Basis.

47

Dias, Bruno, Francisco Maia, Leandro Kerber, João F. C. dos Santos, Eduardo Bica, Tina Armond, Beatriz Barbuy, et al. "The VISCACHA survey – deep and resolved photometry of star clusters in the Magellanic Clouds." Proceedings of the International Astronomical Union 14, S351 (May 2019): 89–92. http://dx.doi.org/10.1017/s174392131900694x.

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AbstractThe VISCACHA (VIsible Soar photometry of star Clusters in tApii and Coxi HuguA†) Survey is an ongoing project based on deep and spatially resolved photometric observations of Magellanic Cloud star clusters, collected using the SOuthern Astrophysical Research (SOAR) telescope together with the SOAR Adaptive Module Imager. So far we have used >300h of telescope time to observe ∼150 star clusters, mostly with low mass (M < 104M⊙) on the outskirts of the LMC and SMC. With this high-quality data set, we homogeneously determine physical properties using deep colour-magnitude diagrams (ages, metallicities, reddening, distances, mass, luminosity and mass functions) and structural parameters (radial density profiles, sizes) for these clusters which are used as a proxy to investigate the interplay between the Magellanic Clouds and their evolution. We present the VISCACHA survey and its initial results, based on our first two papers. The project’s long term goals and expected legacy to the community are also addressed.

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Lampens, Patricia, Jean-Louis Prieur, and Robert Argyle. "Infrared Differential Photometry of Selected Orbital Binaries." International Astronomical Union Colloquium 191 (August 2004): 75–76. http://dx.doi.org/10.1017/s0252921100008514.

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AbstractHigh-angular resolution observations were acquired for a sample of F-G and K nearby orbital binaries, making use of the ADONIS instrument mounted at the 3.6m ESO telescope from La Silla observatory. The aim is to derive broad-band near-infrared colours for the individual components of those binaries which do not fit well the mean mass-luminosity relation, but which have accurate parallaxes (from the Hipparcos satellite) and high-quality orbits, thanks to many previous efforts. Such colour determinations allow component temperatures and photometric mass ratios to be derived.

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Guandalini, R., M. Busso, S. Ciprini, G. Silvestro, and P. Persi. "Infrared photometry and evolution of mass-losing AGB stars." Astronomy & Astrophysics 445, no. 3 (January 2006): 1069–80. http://dx.doi.org/10.1051/0004-6361:20053208.

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Williams, Scott D., John R. Stauffer, Charles F. Prosser, and Terry Herter. "Spectroscopy and photometry for low-mass stars in Praesepe." Publications of the Astronomical Society of the Pacific 106 (August 1994): 817. http://dx.doi.org/10.1086/133448.

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