Comments by Robert J. Silverman on Charles Stansfield's Review of Silverman et al., Oral Language Tests for Bilingual Students (TESOL Quarterly, June 1977)

Silverman, Robert J.

doi:10.2307/3585799

Cited by 25 publications

(46 citation statements)

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“…1 and Sect. 4.1) that the loose self-similarity of SN Ia time series spectra from the perceived beginning of the event to near maximum light was roundly confirmed (Nugent et al 2011, see also Garavini et al 2005;Foley et al 2012c;Silverman et al 2012d;Childress et al 2013c;Zheng et al 2013).…”

Section: Spectramentioning

confidence: 97%

“…Compared to the width of other normal SN Ia B-band light curves, Silverman et al (2012d) find that SN 2012cg's light curve relatively narrow for its peak absolute brightness, with t rise = 17.3 days (coincident photometry was also presented by Munari et al 2013). Mean expansion velocities within 2.5 days of the event were found to be more than 14,000 km s −1 , while the earliest observations show high-velocity components of both Si II and Ca II.…”

Section: A41 Sn 2010jn In Ngc 2929mentioning

confidence: 99%

“…A.43 SN 2012cg in NGC 4424 Silverman et al (2012d) presented early epoch observations of the nearby spectroscopically normal SN 2012cg (Kandrashoff et al 2012;Cenko et al 2012;Marion et al 2012), discovered immediately after the event (∼1.5 days after). Compared to the width of other normal SN Ia B-band light curves, Silverman et al (2012d) find that SN 2012cg's light curve relatively narrow for its peak absolute brightness, with t rise = 17.3 days (coincident photometry was also presented by Munari et al 2013).…”

Section: A41 Sn 2010jn In Ngc 2929mentioning

confidence: 99%

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A review of type Ia supernova spectra

Parrent

Friesen

Parthasarathy

2014

Astrophys Space Sci

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SN 2011fe was the nearest and best-observed type Ia supernova in a generation, and brought previous incomplete datasets into sharp contrast with the detailed new data. In retrospect, documenting spectroscopic behaviors of type Ia supernovae has been more often limited by sparse and incomplete temporal sampling than by consequences of signal-to-noise ratios, telluric features, or small sample sizes. As a result, type Ia supernovae have been primarily studied insofar as parameters discretized by relative epochs and incomplete temporal snapshots near maximum light. Here we discuss a necessary next step toward consistently modeling and directly measuring spectroscopic observables of type Ia supernova spectra. In addition, we analyze current spectroscopic data in the parameter space defined by empirical metrics, which will be relevant even after progenitors are observed and detailed models are refined.

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Section: Spectramentioning

confidence: 97%

Section: A41 Sn 2010jn In Ngc 2929mentioning

confidence: 99%

Section: A41 Sn 2010jn In Ngc 2929mentioning

confidence: 99%

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A review of type Ia supernova spectra

Parrent

Friesen

Parthasarathy

2014

Astrophys Space Sci

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“…In the High-redshift Emission Line Survey (HiZELS) with narrow-band filters in the J, H and K bands, many Hα, [O ii] 3727Å and [O iii] 5007Å emitters have been discovered at 0.4 < z < 2.2 (Geach et al 2008;Sobral et al 2009Sobral et al , 2014Sobral et al , 2015a. The spectroscopic surveys have also been performed and discovered many lines such as C iii] 1909Å, [O ii] 3727Å, [O iii] 5007Å and Hα in the UV to the optical region at z < 3 (Silverman et al 2014;Kashino et al 2014;Nakajima & Ouchi 2014;Stark et al 2014;Sanders et al 2015). Stark et al (2015a) detected C iii] 1909Å emission in two high-z galaxies at z = 6.029 and 7.213.…”

Section: Introductionmentioning

confidence: 99%

Nebular line emission fromz> 7 galaxies in a cosmological simulation: rest-frame UV to optical lines

Shimizu

Inoue

Okamoto

et al. 2016

Mon. Not. R. Astron. Soc.

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We have performed very large and high resolution cosmological hydrodynamic simulations in order to investigate detectability of nebular lines in the rest-frame ultraviolet (UV) to optical wavelength range from galaxies at z > 7. We find that the expected line fluxes are very well correlated with apparent UV magnitudes. The C iv 1549Å and the C iii] 1909Å lines of galaxies brighter than 26 AB are detectable with current facilities such as the VLT/XShooter and the Keck/MOSFIRE. Metal lines such as C iv4959/5007Å can be good targets for the spectroscopic observation with Thirty Meter Telescope (TMT), European Extremely Large Telescope (E-ELT), Giant Magellan Telescope (GMT) and James Webb Space Telescope (JWST). Hα and Hβ lines are also expected to be detectable with these telescopes. We also predict detectability of the nebular lines for z > 10 galaxies that will be found with JWST, Wide-Field Infrared Survey Telescope (WFIRST) and First Light And Reionization Explorer (FLARE) (11 z 15). We conclude that the C iv 1549Å, C iii] 1909Å, [O iii] 4959/5007Å and Hβ lines even from z ∼ 15 galaxies can be strong targets for TMT, ELT and JWST. We also find that the magnification by gravitational lensing is of great help to detect such high-z galaxies. According to our model, the C iii] 1909Å line in z > 9 galaxy candidates is detectable even using the current facilities.

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“…Multi-wavelength spectroscopic follow-up of X-ray selected sources based on Chandra Steffen et al 2004) and XMM-Newton (Barcons et al 2002;Barcons et al 2003;Della Ceca et al 2002;Della Ceca et al 2004) source catalogs have already investigated a number of important astronomical issues such as redshift evolution of Corresponding author: hz@mssl.ucl.ac.uk different classes of Active Galactic Nuclei (AGN) (Miyaji et al 2000;Barger et al 2001a;Komossa & Hasinger 2002;Brandt & Kaspi 2003;Cowie et al 2003;Bauer et al 2004), their intrinsic absorption (Kim & Elvis 1999;Wilkes 2002;Comastri et al 2002;Matt et al 2003) and their relationship with the characteristics of the host galaxy, its star formation history (Ghosh 2002;Sipior et al 2003;Cohen 2003;King 2004;Norman et al 2004;Silverman et al 2005) and the central super-massive black hole (Barger et al 2001b;Granato et al 2002;Brandt et al 2002). Observations have also revealed the relation between hard X-ray sources, hidden broad line AGN (BLAGN) or BL Lac (Ueda et al 2003;Comastri et al 2003;Piconcelli et al 2003) and X-ray background in hard (Gandhi & Fabian 2003;Giacconi et al 2001;Tozzi et al 2001;De Luca & Molendi 2004;Silva et al 2004) and soft bands (Soltan et al 2005).…”

Section: Introductionmentioning

confidence: 99%

Statistical algorithms for identification of astronomical X‐ray sources

Ziaeepour¹,

Rosen²

2008

Astron Nachr

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Observations of present and future X-ray telescopes include a large number of ipitous sources of unknown types. They are a rich source of knowledge about X-ray dominated astronomical objects, their distribution, and their evolution. The large number of these sources does not permit their individual spectroscopical follow-up and classification. Here we use Chandra Multi-Wavelength public data to investigate a number of statistical algorithms for classification of X-ray sources with optical imaging follow-up. We show that up to statistical uncertainties, each class of X-ray sources has specific photometric characteristics that can be used for its classification. We assess the relative and absolute performance of classification methods and measured features by comparing the behaviour of physical quantities for statistically classified objects with what is obtained from spectroscopy. We find that among methods we have studied, multi-dimensional probability distribution is the best for both classifying source type and redshift, but it needs a sufficiently large input (learning) data set. In absence of such data, a mixture of various methods can give a better final result. We discuss some of potential applications of the statistical classification and the enhancement of information obtained in this way. We also assess the effect of classification methods and input data set on the astronomical conclusions such as distribution and properties of X-ray selected sources.

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Comments by Robert J. Silverman on Charles Stansfield's Review of Silverman et al., Oral Language Tests for Bilingual Students (TESOL Quarterly, June 1977)

Cited by 25 publications

References 0 publications

A review of type Ia supernova spectra

A review of type Ia supernova spectra

Nebular line emission fromz> 7 galaxies in a cosmological simulation: rest-frame UV to optical lines

Statistical algorithms for identification of astronomical X‐ray sources

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