<i>K</i>-Sample Anderson–Darling Tests

Scholz, Fritz; Stephens, M. A.

doi:10.1080/01621459.1987.10478517

Cited by 432 publications

(406 citation statements)

References 15 publications

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“…Notably, this function has virtually no dependence on the brightness of the galaxy: the distribution of rest-frame [O ii] equivalent widths for the ∼8500 galaxies discovered in the Las Campanas Redshift Survey is almost independent of R-band luminosity (Blanton & Lin 2000). Similarly, there is no evidence for a correlation between luminosity and equivalent width in an Hα grism-survey of the local universe: if we divide the 191 galaxies of the Gallego et al (1996) survey in half and perform an Anderson-Darling test (Scholz & Stephens 1987), we find no statistical difference between the distributions of [O ii] equivalent widths for the high-and low-line luminosity samples. Figure 1 displays the rest-frame [O ii] equivalent width distribution for the HETDEX pilot survey's sample of emissionline galaxies, as a function of redshift and [O ii] luminosity.…”

Section: The Equivalent Width Distributionmentioning

confidence: 99%

THE HETDEX PILOT SURVEY. IV. THE EVOLUTION OF [O II] EMITTING GALAXIES FROMz∼ 0.5 TOz∼ 0

Ciardullo

Grönwall

Adams

et al. 2013

ApJ

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We present an analysis of the luminosities and equivalent widths of the 284 z < 0.56 [O ii]-emitting galaxies found in the 169 arcmin 2 pilot survey for the Hobby-Eberly Telescope Dark Energy Experiment (HETDEX). By combining emission-line fluxes obtained from the Mitchell spectrograph on the McDonald 2.7 m telescope with deep broadband photometry from archival data, we derive each galaxy's dereddened [O ii] λ3727 luminosity and calculate its total star formation rate. We show that over the last ∼5 Gyr of cosmic time, there has been substantial evolution in the [O ii] emission-line luminosity function, with L * decreasing by ∼0.6 ± 0.2 dex in the observed function, and by ∼0.9 ± 0.2 dex in the dereddened relation. Accompanying this decline is a significant shift in the distribution of [O ii] equivalent widths, with the fraction of high equivalent-width emitters declining dramatically with time. Overall, the data imply that the relative intensity of star formation within galaxies has decreased over the past ∼5 Gyr, and that the star formation rate density of the universe has declined by a factor of ∼2.5 between z ∼ 0.5 and z ∼ 0. These observations represent the first [O ii]-based star formation rate density measurements in this redshift range, and foreshadow the advancements which will be generated by the main HETDEX survey.

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Section: The Equivalent Width Distributionmentioning

confidence: 99%

THE HETDEX PILOT SURVEY. IV. THE EVOLUTION OF [O II] EMITTING GALAXIES FROMz∼ 0.5 TOz∼ 0

Ciardullo

Grönwall

Adams

et al. 2013

ApJ

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“…The size distributions for these samples are shown in Figure 7, which shows them to be virtually identical. A ksample Anderson-Darling (A-D) test (Scholz & Stephens 1987) does not provide strong evidence for the distributions being statistically different.…”

Section: Physical Properties Of Bubble-associated Versus Field Clumpsmentioning

confidence: 99%

The Milky Way Project and Atlasgal: The Distribution and Physical Properties of Cold Clumps Near Infrared Bubbles

Kendrew

Beuther

Simpson

et al. 2016

ApJ

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We present a statistical study of the distribution and physical properties of cold, dense material in and around the inner Galactic Plane near-infrared bubbles as cataloged by the Milky Way Project citizen scientists. Using data from the Atacama Pathfinder Experiment (APEX) Telescope Large Area Survey of the Galaxy 870 μmsurvey, we show that 48±2% of all cold clumps in the studied survey region) are found in close proximity to a bubble, and 25±2% appear directly projected toward a bubble rim. A two-point correlation analysis confirms the strong correlation of massive cold clumps with expanding bubbles. It shows an overdensity of clumps along bubble rims that grows with increasing bubble size, which shows how interstellar medium material is reordered on large scales by bubble expansion around regions of massive star formation. The highest column density clumps appear to be resistent to the expansion, remaining overdense toward the bubbles' interior rather than being swept up by the expanding edge. Spectroscopic observations in ammonia show that cold dust clumps near bubbles appear to be denser, hotter, and more turbulent than those in the field, offering circumstantial evidence that bubble-associated clumps are more likely to be forming stars. These observed differences in physical conditions persist beyond the region of the bubble rims.

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“…We also perform a k-sample Anderson-Darling test (Scholz & Stephens 1987) on the same parameters of Figure 4 to assess whether the tail of the cumulative distributions can affect our results. We find that the null hypothesis that the dispersion sample and the full red-sequence samples are drawn from the same distribution in magnitude and stellar mass can be rejected at 1% and 5% for XMM2235, ∼20% for XMM2215, and 2% and 5% for Cl0332.…”

Section: Distribution Of Galaxy Properties and Selection Effectsmentioning

confidence: 99%

The KMOS Cluster Survey (KCS). I. The Fundamental Plane and the Formation Ages of Cluster Galaxies at Redshift 1.4 < Z < 1.6*

Beifiori

Mendel

Chan

et al. 2017

ApJ

106

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We present the analysis of the fundamental plane (FP) for a sample of 19 massive red-sequence galaxies (M > 4 × 10 10 M ) in 3 known overdensities at 1.39 < z < 1.61 from the KMOS Cluster Survey, a guaranteed time program with spectroscopy from the K-band Multi-Object Spectrograph (KMOS) at the VLT and imaging from the Hubble Space Telescope. As expected, we find that the FP zero-point in B band evolves with redshift, from the value 0.443 of Coma to −0.10 ± 0.09, −0.19 ± 0.05, −0.29 ± 0.12 for our clusters at z = 1.39, z = 1.46, and z = 1.61, respectively. For the most massive galaxies (log M /M > 11) in our sample, we translate the FP zero-point evolution into a mass-to-light-ratio M/L evolution finding ∆ log M/L B = (−0.46 ± 0.10)z, ∆ log M/L B = (−0.52 ± 0.07)z, to ∆ log M/L B = (−0.55 ± 0.10)z, respectively. We assess the potential contribution of the galaxies structural and stellar velocity dispersion evolution to the evolution of the FP zeropoint and find it to be ∼6-35% of the FP zero-point evolution. The rate of M/L evolution is consistent with galaxies evolving passively. By using single stellar population models, we find an average age of 2.33 +0.86 −0.51 Gyr for the log M /M > 11 galaxies in our massive and virialized cluster at z = 1.39, 1.59 +1.40 −0.62 Gyr in a massive but not virialized cluster at z = 1.46, and 1.20 +1.03 −0.47 Gyr in a protocluster at z = 1.61. After accounting for the difference in the age of the Universe between redshifts, the ages of the galaxies in the three overdensities are consistent within the errors, with possibly a weak suggestion that galaxies in the most evolved structure are older.

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K-Sample Anderson–Darling Tests

Cited by 432 publications

References 15 publications

THE HETDEX PILOT SURVEY. IV. THE EVOLUTION OF [O II] EMITTING GALAXIES FROMz∼ 0.5 TOz∼ 0

THE HETDEX PILOT SURVEY. IV. THE EVOLUTION OF [O II] EMITTING GALAXIES FROMz∼ 0.5 TOz∼ 0

The Milky Way Project and Atlasgal: The Distribution and Physical Properties of Cold Clumps Near Infrared Bubbles

The KMOS Cluster Survey (KCS). I. The Fundamental Plane and the Formation Ages of Cluster Galaxies at Redshift 1.4 < Z < 1.6*

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