The Two Micron All Sky Survey (2MASS)

Skrutskie, Michael F.; Cutri, R. M.; Stiening, R.; Weinberg, Martin D.; Schneider, Stephen E.; Carpenter, John M.; Beichman, Charles; Capps, R. W.; Chester, T. J.; Elias, J. H.; Huchra, J. P.; Liebert, James; Lonsdale, C. J.; Monet, D. G.; Price, S.; Seitzer, Patrick; Jarrett, T. H.; Kirkpatrick, J. Davy; Gizis, John E.; Howard, Eric M.; Evans, T. M.; Fowler, J. W.; Fullmer, L.; Hurt, Robert L.; Light, R. M.; Kopan, E. L.; Marsh, Ken; McCallon, H.; Tam, Raymond; Dyk, Schuyler D. Van; Wheelock, S.

doi:10.1086/498708

Cited by 10,368 publications

(6,618 citation statements)

References 16 publications

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“…The relation between equivalent width and interstellar reddening from [30] provides E(B-V) = 0.04 ± 0.01 which we adopt. Using the infrared flux method for the BVJHK system 31 (BV photometry from APASS 32 ; JHK from 2MASS 33 ) we derive a photometric temperature of T eff = 5,210 ± 64 K. From utilisation of griJHK 31 (gri from APASS) we determine T eff = 5,265 ± 76 K. These values and those determined through spectrophotometric analysis are in concordance.…”

supporting

confidence: 54%

A single low-energy, iron-poor supernova as the source of metals in the star SMSS J031300.36−670839.3

Keller

Bessell

Frebel

et al. 2014

Nature

359

401

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The element abundance ratios of four low-mass stars with extremely low metallicities indicate that the gas out of which the stars formed was enriched in each case by at most a few, and potentially only one low-energy, supernova 1,2,3,4 . Such supernovae yield large quantities of light elements such as carbon but very little iron. The dominance of lowenergy supernovae is surprising, because it has been expected that the first stars were extremely massive, and that they disintegrated in pair-instability explosions that would rapidly enrich galaxies in iron 5 . What has remained unclear is the yield of iron from the first supernovae, because hitherto no star is unambiguously interpreted as encapsulating the yield of a single supernova. Here we report the optical spectrum of SMSS J031300.36-670839.3, which shows no evidence of iron (with an upper limit of 10 -7.1 times solar abundance). Based on a comparison of its abundance pattern with those of models, we conclude that the star was seeded with material from a single supernova with an original mass of ~60 M  (and that the supernova left behind a black hole). Taken together with the previously mentioned low-metallicity stars, we conclude that low-energy supernovae were

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supporting

confidence: 54%

A single low-energy, iron-poor supernova as the source of metals in the star SMSS J031300.36−670839.3

Keller

Bessell

Frebel

et al. 2014

Nature

359

401

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“…Cluster fundamental parameters are derived using 2MASS 1 photometry (Skrutskie et al 2006) in the J, H and Ks bands, extracted in circular concentric regions centred on the coordinates given in Table 1 and fitted with PARSEC isochrones (Bressan et al 2012). The fits are made by eye, taking the combined MS and PMS stellar distributions as constraints, and allowing for variations due to photometric uncertainties and differential reddening.…”

Section: Methods Of Analysismentioning

confidence: 99%

Tracing the Galactic spiral structure with embedded clusters

Camargo

Bonatto

Bica

2015

Monthly Notices of the Royal Astronomical Society

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In the present work we investigate the properties of 18 embedded clusters (ECs). The sample includes 11 previously known clusters and we report the discovery of 7 ECs on WISE images, thus complementing our recent list of 437 new clusters. The main goal is to use such clusters to shed new light on the Galactic structure by tracing the spiral arms with cluster distances. Our results favour a four-armed spiral pattern tracing three arms, Sagitarius-Carina, Perseus, and the Outer arm. The SagitariusCarina spiral arm is probed in the borderline of the third and fourth quadrants at a distance from the Galactic centre of d 1 ∼ 6.4 kpc adopting R ⊙ = 7.2 kpc, or d 2 ∼ 7.2 kpc for R ⊙ = 8.0 kpc. Most ECs in our sample are located in the Perseus arm that is traced in the second and third quadrants and appear to be at Galactocentric distances in the range d 1 = 9 − 10.5 kpc or d 2 = 9.8 − 11.3 kpc. Dolidze 25, Bochum 2, and Camargo 445 are located in the Outer arm that extends along the second and third Galactic quadrants with a distance from the Galactic centre in the range of d 1 = 12.5 − 14.5 kpc or d 2 = 13.5 − 15.5 kpc. We find further evidence that in the Galaxy ECs are predominantly located within the thin disc and along spiral arms. They are excellent tools for tracing these Galactic features and therefore new searches for ECs can contribute to a better understanding of the Galactic structure. We also report an EC aggregate located in the Perseus arm.

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“…We therefore do not expect a large velocity offset > 100 km s −1 between the gas structures and the stellar potential. Skrutskie et al 2006). Bottom: CO(3-2) integrated intensity map for velocities −240 to 180 km s −1 .…”

Section: Velocity Structurementioning

confidence: 99%

“…We have considered both estimates of the total mass in our analysis. The scale radius of 10 kpc was estimated from the K-band effective radius of 9.5 arcsec given by the 2MASS extended source catalogue 2 (Skrutskie et al 2006). We note that this may underestimate the true value as the 2MASS observations are not deep enough to trace the full extent of the BCG envelope and PKS 0745-191 lies near the Galactic plane on the sky.…”

Section: Molecular Gas Clouds In Gravitational Free-fall?mentioning

confidence: 99%

ALMA observations of cold molecular gas filaments trailing rising radio bubbles in PKS 0745−191

Russell

McNamara

Fabian

et al. 2016

Mon. Not. R. Astron. Soc.

105

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We present ALMA observations of the CO(1-0) and CO(3-2) line emission tracing filaments of cold molecular gas in the central galaxy of the cluster PKS 0745-191. The total molecular gas mass of 4.6±0.3×10 9 M , assuming a Galactic X CO factor, is divided roughly equally between three filaments each extending radially 3 − 5 kpc from the galaxy centre. The emission peak is located in the SE filament ∼ 1 arcsec (2 kpc) from the nucleus. The velocities of the molecular clouds in the filaments are low, lying within ±100 km s −1 of the galaxy's systemic velocity. Their FWHMs are less than 150 km s −1 , which is significantly below the stellar velocity dispersion. Although the molecular mass of each filament is comparable to a rich spiral galaxy, such low velocities show that the filaments are transient and the clouds would disperse on < 10 7 yr timescales unless supported, likely by the indirect effect of magnetic fields. The velocity structure is inconsistent with a merger origin or gravitational free-fall of cooling gas in this massive central galaxy. If the molecular clouds originated in gas cooling even a few kpc from their current locations their velocities would exceed those observed. Instead, the projection of the N and SE filaments underneath X-ray cavities suggests they formed in the updraft behind bubbles buoyantly rising through the cluster atmosphere. Direct uplift of the dense gas by the radio bubbles appears to require an implausibly high coupling efficiency. The filaments are coincident with low temperature X-ray gas, bright optical line emission and dust lanes indicating that the molecular gas could have formed from lifted warmer gas that cooled in situ.

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The Two Micron All Sky Survey (2MASS)

Cited by 10,368 publications

References 16 publications

A single low-energy, iron-poor supernova as the source of metals in the star SMSS J031300.36−670839.3

A single low-energy, iron-poor supernova as the source of metals in the star SMSS J031300.36−670839.3

Tracing the Galactic spiral structure with embedded clusters

ALMA observations of cold molecular gas filaments trailing rising radio bubbles in PKS 0745−191

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