JHKLM photometry: Standard systems, passbands and intrinsic colors

Bessell, M. S.; Brett, J. M.

doi:10.1007/3-540-51610-7_8

Cited by 21 publications

(25 citation statements)

References 8 publications

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“…For the M stars, infrared magnitudes allow for discrimination between dwarfs and giants. 18 G and K dwarfs are distinguished from giants through their relatively rapid reduced proper motion. 19 It may also be possible to use trigonometric parallaxes measured by the ongoing European "Gaia" mission, if they become available early enough for TESS mission planning.…”

Section: Star Selectionmentioning

confidence: 99%

Transiting Exoplanet Survey Satellite

Ricker

Winn

Vanderspek

et al. 2014

J. Astron. Telesc. Instrum. Syst

3,030

1,691

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Abstract. The Transiting Exoplanet Survey Satellite (TESS) will search for planets transiting bright and nearby stars. TESS has been selected by NASA for launch in 2017 as an Astrophysics Explorer mission. The spacecraft will be placed into a highly elliptical 13.7-day orbit around the Earth. During its 2-year mission, TESS will employ four wide-field optical charge-coupled device cameras to monitor at least 200,000 main-sequence dwarf stars with I C ≈ 4 − 13 for temporary drops in brightness caused by planetary transits. Each star will be observed for an interval ranging from 1 month to 1 year, depending mainly on the star's ecliptic latitude. The longest observing intervals will be for stars near the ecliptic poles, which are the optimal locations for follow-up observations with the James Webb Space Telescope. Brightness measurements of preselected target stars will be recorded every 2 min, and full frame images will be recorded every 30 min. TESS stars will be 10 to 100 times brighter than those surveyed by the pioneering Kepler mission. This will make TESS planets easier to characterize with follow-up observations. TESS is expected to find more than a thousand planets smaller than Neptune, including dozens that are comparable in size to the Earth. Public data releases will occur every 4 months, inviting immediate community-wide efforts to study the new planets. The TESS legacy will be a catalog of the nearest and brightest stars hosting transiting planets, which will endure as highly favorable targets for detailed investigations. © The Authors. Published by SPIE under a Creative Commons Attribution 3.0 Unported License. Distribution or reproduction of this work in whole or in part requires full attribution of the original publication, including its DOI.

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Section: Star Selectionmentioning

confidence: 99%

Transiting Exoplanet Survey Satellite

Ricker

Winn

Vanderspek

et al. 2014

J. Astron. Telesc. Instrum. Syst

3,030

1,691

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“…To obtain synthetic light curves which illustrate the complete evolution of the emitted radiation during the photospheric phase of our model, we integrate these over the appropriate filter functions 43,44 .…”

Section: Radiative Transfer Simulationsmentioning

confidence: 99%

Sub-luminous type Ia supernovae from the mergers of equal-mass white dwarfs with mass ∼0.9M⊙

Pakmor

Kromer

Röpke

et al. 2010

Nature

377

475

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, a mass of 0.89 M ʘ , a composition of equal parts by mass of carbon and oxygen and an initial temperature of 5× 10 5 K. The initial orbit is circular with a period of 28s. This corresponds to the state when tidal forces deform the white dwarfs sufficiently to make the system unstable (prior evolution is driven by gravitational wave emission and is not simulated). This progenitor system is set up as the initial conditions for a simulation using a smoothed particle hydrodynamics code 12 (SPH). In the initial conditions, marginal asymmetries were deliberately introduced since perfect symmetry is not expected in Nature. In this first simulation, we follow the 3 inspiral and subsequent merger of the binary system (Figure 1). After two orbits one of the two white dwarfs is disrupted. This unequal evolution of the white dwarfs originates from the symmetry-breaking in the initial conditions. The disrupted white dwarf violently merges with the remaining white dwarf and material is heated by compression.In the hottest regions carbon burning begins and releases additional energy which further heats the material. A hotspot, which is resolved by several SPH particles, forms with a temperature of 2.9× 10 9 K in high-density material (3.8× 10 6 g cm -3). Highresolution small-scale simulations 13 show that under such conditions a detonation ignites.In the second step of our simulation sequence, we impose the triggering of a detonation at the hottest point and follow it with a grid-based hydrodynamics code 14,15 as it crosses the merged object. The energy release from the nuclear burning in the detonation disrupts the system (see Figure 1) Finally, we use the structure of the ejecta and the detailed chemical abundances to calculate synthetic light curves and spectra using a Monte Carlo radiative transfer code 19 as required to quantitatively test this model against observations. Owing to the small 56 Ni mass synthesized during the nuclear burning, the synthetic light curves (Figure 2) are faint and decline rapidly compared to those of normal SNe Ia, despite the large total ejecta mass of our simulation (1.8 M ʘ ). Given that there has been no fine-tuning of the explosion model, the light curves agree remarkably well with those of the 1991bg-like SNe Ia -in both absolute magnitude and colour evolution. Moreover, our model naturally predicts the lack of secondary maxima in the near-infrared (J, H and K) light curves which is a peculiarity of 1991bg-like objects compared to normal SNe Ia.In detail, however, there are some discrepancies between our model light curves and the observational data. Comparing the difference in brightness at B band maximum and 15 days thereafter we find values between 1.4 and 1.7 -depending on the line-ofsight. This is less than typically observed for 1991bg-like objects (1.9), but at worst similar to the fastest declining normal SNe Ia and substantially faster than for objects which have previously been claimed as possible super-Chandrasekhar explosions (e.g. The total mass of the system is essential...

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“…For the M stars, infrared magnitudes allow for discrimination between dwarfs and giants. 19 G and K dwarfs are distinguished from giants through their relatively rapid reduced proper motion. 20 It may also be possible to use trigonometric parallaxes measured by the ongoing European Gaia mission, if they become available early enough for TESS mission planning.…”

mentioning

confidence: 99%

Transiting Exoplanet Survey Satellite (TESS)

Ricker

Winn²,

Vanderspek³

et al. 2014

SPIE Proceedings

746

288

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The Transiting Exoplanet Survey Satellite (TESS ) will search for planets transiting bright and nearby stars. TESS has been selected by NASA for launch in 2017 as an Astrophysics Explorer mission. The spacecraft will be placed into a highly elliptical 13.7-day orbit around the Earth. During its two-year mission, TESS will employ four wide-field optical CCD cameras to monitor at least 200,000 main-sequence dwarf stars with I C < ∼ 13 for temporary drops in brightness caused by planetary transits. Each star will be observed for an interval ranging from one month to one year, depending mainly on the star's ecliptic latitude. The longest observing intervals will be for stars near the ecliptic poles, which are the optimal locations for follow-up observations with the James Webb Space Telescope. Brightness measurements of preselected target stars will be recorded every 2 min, and full frame images will be recorded every 30 min. TESS stars will be 10-100 times brighter than those surveyed by the pioneering Kepler mission. This will make TESS planets easier to characterize with follow-up observations. TESS is expected to find more than a thousand planets smaller than Neptune, including dozens that are comparable in size to the Earth. Public data releases will occur every four months, inviting immediate community-wide efforts to study the new planets. The TESS legacy will be a catalog of the nearest and brightest stars hosting transiting planets, which will endure as highly favorable targets for detailed investigations.

show abstract

JHKLM photometry: Standard systems, passbands and intrinsic colors

Cited by 21 publications

References 8 publications

Transiting Exoplanet Survey Satellite

Transiting Exoplanet Survey Satellite

Sub-luminous type Ia supernovae from the mergers of equal-mass white dwarfs with mass ∼0.9M⊙

Transiting Exoplanet Survey Satellite (TESS)

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