Universality of the Near-Infrared Extinction Law Based on the Apogee Survey

Wang, Shu; Jiang, Biwei

doi:10.1088/2041-8205/788/1/l12

Cited by 75 publications

(104 citation statements)

References 34 publications

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“…Several recent studies (Nishiyama et al 2009;Fitzpatrick & Massa 2009;Stead & Hoare 2009;Schödel et al 2010;Fritz et al 2011;Wang & Jiang 2014) have demonstrated such power law with exponents α ≈ 2 is suitable for the Galactic extinction in the near infrared. Since we can calculate the extinction index A K based on two different color indexes (J − K and H − K) for Mc20, we can establish α as the value that matches both extinction calculations for each star.…”

Section: Extinction and Distancementioning

confidence: 95%

First detections of FS Canis Majoris stars in clusters

Fuente

Najarro

Trombley

et al. 2015

A&A

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Context. FS CMa stars are low-luminosity objects showing the B[e] phenomenon whose evolutionary state remains a puzzle. These stars are surrounded by compact disks of warm dust of unknown origin. Hitherto, membership of FS CMa stars to coeval populations has never been confirmed. Aims. The discovery of low-luminosity line emitters in the young massive clusters Mercer 20 and Mercer 70 prompts us to investigate the nature of such objects. We intend to confirm membership to coeval populations in order to characterize these emission-line stars through the cluster properties.

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Section: Extinction and Distancementioning

confidence: 95%

First detections of FS Canis Majoris stars in clusters

Fuente

Najarro

Trombley

et al. 2015

A&A

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“…Compared to shorter (optical) and longer (MIR) wavelengths, the extinction curve is considered relatively constant in the NIR regime (e.g. Indebetouw et al 2005;Lombardi et al 2006;Román-Zúñiga et al 2007;Ascenso et al 2013;Wang & Jiang 2014) and the power-law slope of the NIR extinction curve typically only varies at a level of ∼5% (Stead & Hoare 2009;Fritz et al 2011). In very dense cores the formation of ice mantles and the grain growth could have an additional impact.…”

Section: Comparison With Other Studiesmentioning

confidence: 99%

Galactic cold cores

Juvela

Ristorcelli

Marshall

et al. 2015

A&A

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Context. The project Galactic Cold Cores has carried out Herschel photometric observations of interstellar clouds where the Planck satellite survey has located cold and compact clumps. The sources represent different stages of cloud evolution from starless clumps to protostellar cores and are located in different Galactic environments. Aims. We examine this sample of 116 Herschel fields to estimate the submillimetre dust opacity and to search for variations that might be attributed to the evolutionary stage of the sources or to environmental factors, including the location within the Galaxy. Methods. The submillimetre dust opacity was derived from Herschel data, and near-infrared observations of the reddening of background stars are converted into near-infrared optical depth. We investigated the systematic errors affecting these parameters and used modelling to correct for the expected biases. The ratio of 250 μm and J band opacities is correlated with the Galactic location and the star formation activity. We searched for local variations in the ratio τ(250 μm)/τ(J) using the correlation plots and opacity ratio maps. Results. We find a median ratio of τ(250 μm)/τ(J) = (1.6 ± 0.2) × 10 −3 , which is more than three times the mean value reported for the diffuse medium. Assuming an opacity spectral index β = 1.8 instead of β = 2.0, the value would be lower by ∼30%. No significant systematic variation is detected with Galactocentric distance or with Galactic height. Examination of the τ(250 μm)/τ(J) maps reveals six fields with clear indications of a local increase of submillimetre opacity of up to τ(250 μm)/τ(J) ∼ 4 × 10 −3 towards the densest clumps. These are all nearby fields with spatially resolved clumps of high column density. Conclusions. We interpret the increase in the far-infrared opacity as a sign of grain growth in the densest and coldest regions of interstellar clouds.

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“…For example, the CCM extinction curve contains no variation in the infrared, while the extinction curve of Fitzpatrick & Massa (2009) is more variable in the NIR than in the red-optical. Different authors have found both "universal" NIR extinction (e.g., Wang & Jiang 2014) and variable infrared extinction (e.g., Zasowski et al 2009). Meanwhile optical studies essentially always find extinction curve variability, though often with the caveat that "most" extinction curves are compatible with an "average" Milky Way extinction curve (e.g., Krełowski & Strobel 2012).…”

Section: Introductionmentioning

confidence: 99%

“…Many studies of the extinction curve have focused on only a small range of wavelengths for practical reasons, for example, focusing either on only the optical (e.g., Schlafly et al 2010) or only the near-infrared (NIR) (e.g., Wang & Jiang 2014) extinction curve. This means that individual parts of the extinction curve are known much better than the connections between these parts.…”

Section: Introductionmentioning

confidence: 99%

The Optical–infrared Extinction Curve and Its Variation in the Milky Way

Schlafly

Meisner

Stutz

et al. 2016

ApJ

249

278

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The dust extinction curve is a critical component of many observational programs and an important diagnostic of the physics of the interstellar medium. Here we present new measurements of the dust extinction curve and its variation toward tens of thousands of stars, a hundred-fold larger sample than in existing detailed studies. We use data from the APOGEE spectroscopic survey in combination with ten-band photometry from Pan-STARRS1, the Two Micron All-Sky Survey, and Wide-field Infrared Survey Explorer. We find that the extinction curve in the optical through infrared is well characterized by a one-parameter family of curves described by R(V). The extinction curve is more uniform than suggested in past works, with ( ( )) s = R V 0.18, and with less than one percent of sight lines having ( ) > R V 4. Our data and analysis have revealed two new aspects of Galactic extinction: first, we find significant, wide-area variations in R(V) throughout the Galactic plane. These variations are on scales much larger than individual molecular clouds, indicating that R(V) variations must trace much more than just grain growth in dense molecular environments. Indeed, we find no correlation between R(V) and dust column density up to ( ) -» E B V 2. Second, we discover a strong relationship between R(V) and the far-infrared dust emissivity.

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Universality of the Near-Infrared Extinction Law Based on the Apogee Survey

Cited by 75 publications

References 34 publications

First detections of FS Canis Majoris stars in clusters

First detections of FS Canis Majoris stars in clusters

Galactic cold cores

The Optical–infrared Extinction Curve and Its Variation in the Milky Way

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