Dataset for: "Spatial Variation in Strong Line Ratios and Physical Conditions in Two Strongly-Lensed Galaxies at z~1.4"
Michael FlorianJane R. RigbyAyan AcharyyaKeren SharonMichael D. GladdersLisa J. KewleyGourav KhullarKatya GozmanGabriel BrammerIvelina MomchevaDavid C. NichollsStephanie LaMassaH. DahleMatthew BaylissEva WuytsTraci L. JohnsonKatherine E. Whitaker
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Abstract:
This repository deposit contains the 1D HST WFC3-IR grism spectra used in the accepted version of the manuscript "Spatial Variation in Strong Line Ratios and Physical Conditions in Two Strongly-Lensed Galaxies at z~1.4" (accepted 08-Apr-2021). There are 20 spectra included in this deposit. They are listed here with basic information about each file. In the table below, "bothroll" refers to stacks of spectra from both roll angles while "roll139" denotes spectra using only the 139 degree roll angle (this only applies to the smaller, complete image 2 of sgas1723). For the target sgas2340, "4stackednoim3" refers to a stack of spectra of 4 of the complete images, namely images 1,2, and 4 from the 043 degree roll angle and image 1 from the 327 degree roll angle. For spectra of regions within sgas2340, strings such as "A1A2A4A1" denote, for example, that spectra from images A1, A2, and A4 from one roll angle were used and only the image A1 from the second roll angle was used. See figure 1 and table 2. These spectra are neither continuum-subtracted, corrected for Milky Way reddening, nor corrected for reddening from dust within these targets.Keywords:
Variation (astronomy)
Line (geometry)
Firstly,according to variation contents,the paper divides variation into operating range variation,construction condition variation,design variation,construction variation and technique standards variation. Contraposing to different content variation,the paper puts forward dissimilar control methods. According to the property of project variation,the paper divides variation into fatal variation,important variation and general variation,and points out that we can control variation effectively by establishing dissimilar authority of project variation examination and approval. Finally,according to the urgency of variation,the paper divides variation into variation under urgent circumstance and variation under not urgent circumstance,and puts forward that we can control these variation by different procedure.
Variation (astronomy)
Process Variation
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AbstractThe names of 1024 American automobiles are analyzed according to register variation, diachronic variation and manufacturer variation. Variation through such linguistic means as structural complexity, metonymy and iconicity is shown to not only reflect social realities of automobile producers and consumers but to actively contribute to constructing these realities as well.
Variation (astronomy)
Iconicity
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Variation is an important issue of sociolinguistics.According to the variation view of sociolinguistics,grammatical items change under the influence of social factors.Compared with the research on phonetic variation,the research on grammatical variation is weaker.This article presents a review of the literature both at home and abroad on grammatical or syntactic variation.Some propositions for Chinese researchers on grammatical or syntactic variation are put forward at the end of the paper.
Variation (astronomy)
Sociolinguistics
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Variation occurs when a language has two or more ways of achieving the same communicative goal. Cases of variation have been approached in very different ways by two different groups of linguists. Variationists assume that variation is natural and common. On this view, change is due to naturally occurring variation interacting with language-external forces. Functionalists assume that variation is anomalous. On this view, change may reflect a language-internal drive to eradicate variation. In this paper, it is argued that these conflicting views can be reconciled by considering how variation functions in the broader context of the grammar. Drawing on a case study into the prepositional complements following emotion adjectives, it is proposed that variation (as Variationists maintain) is natural and that languages have no intrinsic tendency to reduce variability. Nevertheless, the synchronic availability and historical development of specific variants is (as Functionalists maintain) also internally motivated, typically by analogical relations.
Variation (astronomy)
Language Change
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Empirical and experimental work has yielded burgeoning evidence of intra-individual variation drawing on a variety of analytical frameworks and methodological approaches. A systematic review of intra-individual variation is thus timely both to provide guidance for researchers wishing to interpret and understand intra-individual variation and to provide some theoretical and methodological resources to evaluate the rapidly growing body of literature on intra-individual variation. The present chapter thus untangles intra-individual variation both terminologically and conceptually. We survey the scholarly discussion and evaluation of intra-individual variation in the interdisciplinary discourse of theoretical linguistic frameworks and empirical studies. By sketching previous research, we systematise various types of intra-individual and derive the proposal for a model of intra-individual variation followed by some remarks about the application of intra-individual variation.
Variation (astronomy)
Empirical Research
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Cross-talks and sketches are two important forms of language art in our country. They are popular with a wide range of audiences around the country due to their humorous language. Language variation is a very important means of creating humor effect. In cross-talks and sketches,various forms of language variation, including phonetic variation, lexical variation,grammar variation, semantic variation,stylistic variation and pragmatic variation,are applied to realize humor effect.
Variation (astronomy)
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A sensitive observation of the CO J = 1-0 molecular line emission in the host galaxy of GRB 030329 (z = 0.1685) has been performed using the Nobeyama Millimeter Array to detect molecular gas and hidden star formation. No sign of CO emission was found, which invalidates our previous report of the presence of molecular gas. The 3 σ upper limit on the CO line luminosity (L) of the host galaxy is 6.9 × 108 K km s-1 pc2. The lower limit to the host galaxy's metallicity is estimated to be 12 + log (O/H) ~ 7.9, which yields a conversion factor from CO line luminosity to H2 of αCO = 40 M☉ (K km s-1 pc2)-1. Assuming this factor, the 3 σ upper limit on the molecular gas mass of the host galaxy is 2.8 × 1010 M☉. Based on the Schmidt law, the 3 σ upper limit on the total star formation rate (SFR) of the host galaxy is estimated to be 38 M☉ yr-1. These results independently confirm inferences from previous observations in the optical, submillimeter, and X-ray bands, which regard this host galaxy as a compact dwarf and not a massive, aggressively star-forming galaxy. Finally, the SFRs of GRB host galaxies, estimated using various techniques immune to dust obscuration, including our CO luminosity measurements, are compared with the SFRs of the same galaxies estimated using extinction-corrected optical/UV tracers. We show that most of the SFRs measured in extinction-free wavelengths, including positive detections and upper limits, are larger by from 1 to a few orders of magnitude compared with the SFRs of the same galaxies measured by optical/UV tracers.
Extinction (optical mineralogy)
Submillimeter Array
Irregular galaxy
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Variation (astronomy)
Language Change
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The nationally-recognized Susquehanna
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to be moved, to be part of the
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working at an extremely high
musical level.AÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂA¢AÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂAÂA Experience choral
singing that will take you to new
heights!
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The bright, soft X-ray spectrum Seyfert 1 galaxies Ark 564 and Ton S180 were monitored for 35 days and 12 days, respectively, with ASCA and RXTE (and EUVE for Ton S180). These represent the most intensive X-ray monitoring of any such soft-spectrum Seyfert 1 to date. Light curves were constructed for Ton S180 in six bands spanning 0.1-10 keV and for Ark 564 in five bands spanning 0.7-10 keV. The short-timescale (hours-days) variability patterns were very similar across energy bands, with no evidence of lags between any of the energy bands studied. The fractional variability amplitude was almost independent of energy band, unlike hard-spectrum Seyfert 1 galaxies, which show stronger variations in the softer bands. It is difficult to simultaneously explain soft Seyfert galaxies stronger variability, softer spectra, and weaker energy dependence of the variability relative to hard Seyfert galaxies. There was a trend for soft- and hard-band light curves of both objects to diverge on the longest timescales probed (~weeks), with the hardness ratio showing a secular change throughout the observations. This is consistent with the fluctuation power density spectra that showed relatively greater power on long timescales in the softest bands. The simplest explanation of all of these is that two continuum emission components are visible in the X-rays: a relatively hard, rapidly variable component that dominates the total spectrum and a slowly variable soft excess that only shows up in the lowest energy channels of ASCA. Although it would be natural to identify the latter component with an accretion disk and the former with a corona surrounding it, a standard thin disk could not get hot enough to radiate significantly in the ASCA band, and the observed variability timescales are much too short. It also appears that the hard component may have a more complex shape than a pure power law. The most rapid factor of 2 flares and dips occurred within ~1000 s, in Ark 564 and a bit more slowly in Ton S180. The speed of the luminosity changes rules out viscous or thermal processes and limits the size of the individual emission regions to ≲15 Schwarzschild radii (and probably much less), that is, to either the inner disk or small regions in a corona.
Ton
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