Spectral Irradiance Calibration in the Infrared. XIV. The Absolute Calibration of 2MASS

Cohen, Martin; Wheaton, W. A.; Megeath, S. Thomas

doi:10.1086/376474

Cited by 748 publications

(723 citation statements)

References 8 publications

Supporting

Mentioning

699

Contrasting

Order By: Relevance

“…-2: Bessell & Murphy (2012): notice that the formalism introduced in that paper for the U BV(RI) C system is in terms of AB magnitudes, although the system is actually VEGA based; ζ values are obtained from their tables 3 and 5 (but with the opposite sign, following our definition of ζ ). -3: Cohen et al (2003); ζ values from Casagrande et al (2010). -4: SDSS website; ζ values are obtained comparing the observed magnitudes of a number of HST CALSPEC standards with the magnitudes generated in the AB system using the adopted T ζ with the HST absolute spectrophotometry.…”

Section: Bolometric Correctionsmentioning

confidence: 99%

Synthetic stellar photometry – I. General considerations and new transformations for broad-band systems

Casagrande¹,

VandenBerg²

2014

Monthly Notices of the Royal Astronomical Society

263

321

View full text Add to dashboard Cite

After a pedagogical introduction to the main concepts of synthetic photometry, colours and bolometric corrections in the Johnson-Cousins, 2MASS, and HST-ACS/WFC3 photometric systems are generated from MARCS synthetic fluxes for various [Fe/H] and [α/Fe] combinations, and virtually any value of E(B − V) 0.7. The successes and failures of model fluxes in reproducing the observed magnitudes are highlighted. Overall, extant synthetic fluxes predict quite realistic broad-band colours and bolometric corrections, especially at optical and longer wavelengths: further improvements of the predictions for the blue and ultraviolet spectral regions await the use of hydrodynamic models where the microturbulent velocity is not treated as a free parameter. We show how the morphology of the colour-magnitude diagram (CMD) changes for different values of [Fe/H] and [α/Fe]; in particular,how suitable colour combinations can easily discriminate between red giant branch and lower main sequence populations with different [α/Fe], due to the concomitant loops and swings in the CMD. We also provide computer programs to produce tables of synthetic bolometric corrections as well as routines to interpolate in them. These colour-T eff -metallicity relations may be used to convert isochrones for different chemical compositions to various bandpasses assuming observed reddening values, thus bypassing the standard assumption of a constant colour excess for stars of different spectral type. We also show how such an assumption can lead to significant systematic errors. The MARCS transformations presented in this study promise to provide important constraints on our understanding of the multiple stellar populations found in globular clusters (e.g., the colours of lower main sequence stars are predicted to depend strongly on [α/Fe]) and of those located towards/in the Galactic bulge.

show abstract

Section: Bolometric Correctionsmentioning

confidence: 99%

Synthetic stellar photometry – I. General considerations and new transformations for broad-band systems

Casagrande¹,

VandenBerg²

2014

Monthly Notices of the Royal Astronomical Society

263

321

View full text Add to dashboard Cite

show abstract

“…PS1 photometry is on the AB magnitude scale (Tonry et al 2012), calibrated using the procedures outlined in Schlafly et al (2012) and Magnier et al (2013). 2MASS, AllWISE, and Gaia photometry are calibrated on the Vega magnitude scale (Cohen et al 2003;Wright et al 2010;Carrasco et al 2016, respectively).…”

Section: Photometrymentioning

confidence: 99%

Photometry and Proper Motions of M, L, and T Dwarfs from the Pan-STARRS1 3 π Survey

Best

Magnier

Liu

et al. 2017

ApJS

119

110

View full text Add to dashboard Cite

The full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-pro t purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details. AbstractWe present a catalog of 9888 M, L and T dwarfs detected in the Pan-STARRS13π Survey (PS1), covering threequarters of the sky. Our catalog contains nearly all known objects of spectral types L0-T2 in the PS1 field, with objects as early as M0 and as late as T9, and includes PS1, 2MASS, AllWISE, and GaiaDR1 photometry. We analyze the different types of photometry reported by PS1 and use two types in our catalog in order to maximize both depth and accuracy. Using parallaxes from the literature, we construct empirical SEDs for field ultracool dwarfs spanning 0.5-12 μm. We determine typical colors of M0-T9 dwarfs and highlight the distinctive colors of subdwarfs and young objects. We combine astrometry from PS1, 2MASS, and GaiaDR1 to calculate new proper motions for our catalog. We achieve a median precision of 2.9mas yr −1 , a factor of ≈3−10 improvement over previous large catalogs. Our catalog contains proper motions for 2405M6-T9 dwarfs and includes the largest set of homogeneous proper motions for L and T dwarfs published to date, 406objects for which there were no previous measurements, and 1176objects for which we improve upon previous literature values. We analyze the kinematics of ultracool dwarfs in our catalog and find evidence that bluer but otherwise generic late-M and Lfield dwarfs (i.e., not subdwarfs) tend to have tangential velocities higher than those of typical field objects. With the public release of the PS1 data, this survey will continue to be an essential tool for characterizing the ultracool dwarf population.

show abstract

“…We match with 2MASS using a cross-radius of 5″ and find that 90 objects have detections in at least one bandpass. We choose the profile-fit photometry magnitude from the catalog, and convert the Vegabased magnitude to physical flux based on Cohen et al (2003). UKIDSS is another near-IR imaging survey.…”

Section: Near-ir Datamentioning

confidence: 99%

Herschel Observed Stripe 82 Quasars and Their Host Galaxies: Connections Between Agn Activity and Host Galaxy Star Formation

2016

ApJ

View full text Add to dashboard Cite

In this work, we present a study of 207 quasars selected from the Sloan Digital Sky Survey quasar catalogs and the Herschel Stripe 82 survey. Quasars within this sample are high-luminosity quasars with a mean bolometric luminosity of 10 46.4 erg s −1 . The redshift range of this sample is within z < 4, with a mean value of 1.5 ± 0.78. Because we only selected quasars that have been detected in all three Herschel-SPIRE bands, the quasar sample is complete yet highly biased. Based on the multi-wavelength photometric observation data, we conducted a spectral energy distribution (SED) fitting through UV to FIR. Parameters such as active galactic nucleus (AGN) luminosity, far-IR (FIR) luminosity, stellar mass, as well as many other AGN and galaxy properties are deduced from the SED fitting results. The mean star formation rate (SFR) of the sample is 419 M e yr −1 and the mean gas mass is ∼10 11.3 M e . All of these results point to an IR luminous quasar system. Compared with star formation main sequence (MS) galaxies, at least 80 out of 207 quasars are hosted by starburst galaxies. This supports the statement that luminous AGNs are more likely to be associated with major mergers. The SFR increases with the redshift up to z = 2. It is correlated with the AGN bolometric luminosity, where µ  L L FIR Bol 0.46 0.03 . The AGN bolometric luminosity is also correlated with the host galaxy mass and gas mass. Yet the correlation between L FIR and L Bol has higher significant level, implies that the link between AGN accretion and the SFR is more primal. The M BH /M * ratio of our sample is 0.02, higher than the value 0.005 in the local universe. It might indicate an evolutionary trend of the M BH -M * scaling relation.

show abstract

Spectral Irradiance Calibration in the Infrared. XIV. The Absolute Calibration of 2MASS

Cited by 748 publications

References 8 publications

Synthetic stellar photometry – I. General considerations and new transformations for broad-band systems

Synthetic stellar photometry – I. General considerations and new transformations for broad-band systems

Photometry and Proper Motions of M, L, and T Dwarfs from the Pan-STARRS1 3 π Survey

Herschel Observed Stripe 82 Quasars and Their Host Galaxies: Connections Between Agn Activity and Host Galaxy Star Formation

Contact Info

Product

Resources

About