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<jats:title>Abstract</jats:title> <jats:p>We present the second dust continuum data release in the Census of High- and Medium-mass Protostars (CHaMP), expanding the methodology trialed in Pitts et al. to the entire CHaMP survey area (280° &lt; <jats:italic>ℓ</jats:italic> &lt; 300°, − 4° &lt; <jats:italic>b</jats:italic> &lt; + 2°). This release includes maps of dust temperature (<jats:italic>T</jats:italic> <jats:sub>d</jats:sub>), H<jats:sub>2</jats:sub> column density (<jats:inline-formula> <jats:tex-math> <?CDATA ${N}_{{{\rm{H}}}_{2}}$?> </jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msub> <mml:mrow> <mml:mi>N</mml:mi> </mml:mrow> <mml:mrow> <mml:msub> <mml:mrow> <mml:mi mathvariant="normal">H</mml:mi> </mml:mrow> <mml:mrow> <mml:mn>2</mml:mn> </mml:mrow> </mml:msub> </mml:mrow> </mml:msub> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjsac063dieqn1.gif" xlink:type="simple" /> </jats:inline-formula>), gas-phase CO abundance, and temperature–density plots for every prestellar clump with Herschel coverage, showing no evidence of internal heating for most clumps in our sample. We show that CO abundance is a strong function of <jats:italic>T</jats:italic> <jats:sub>d</jats:sub> and can be fit with a second-order polynomial in log-space, with a typical dispersion of a factor of 2–3. The CO abundance peaks at <jats:inline-formula> <jats:tex-math> <?CDATA ${20.0}_{-1.0}^{+0.4}$?> </jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msubsup> <mml:mrow> <mml:mn>20.0</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>1.0</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>0.4</mml:mn> </mml:mrow> </mml:msubsup> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjsac063dieqn2.gif" xlink:type="simple" /> </jats:inline-formula> K with a value of <jats:inline-formula> <jats:tex-math> <?CDATA ${7.4}_{-0.3}^{+0.2}\times {10}^{-5}$?> </jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msubsup> <mml:mrow> <mml:mn>7.4</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>0.3</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>0.2</mml:mn> </mml:mrow> </mml:msubsup> <mml:mo>×</mml:mo> <mml:msup> <mml:mrow> <mml:mn>10</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>5</mml:mn> </mml:mrow> </mml:msup> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjsac063dieqn3.gif" xlink:type="simple" /> </jats:inline-formula> per H<jats:sub>2</jats:sub>; the low <jats:italic>T</jats:italic> <jats:sub>d</jats:sub> at which this maximal abundance occurs relative to laboratory results is likely due to interstellar UV bombardment in the largest survey fields. Finally, we show that, as predicted by theoretical literature and hinted at in previous studies of individual clouds, the conversion factor from integrated <jats:sup>12</jats:sup>CO line intensity (<jats:inline-formula> <jats:tex-math> <?CDATA ${I}_{{}^{12}{\rm{CO}}}$?> </jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msub> <mml:mrow> <mml:mi>I</mml:mi> </mml:mrow> <mml:mrow> <mml:msup> <mml:mrow /> <mml:mrow> <mml:mn>12</mml:mn> </mml:mrow> </mml:msup> <mml:mi mathvariant="normal">CO</mml:mi> </mml:mrow> </mml:msub> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjsac063dieqn4.gif" xlink:type="simple" /> </jats:inline-formula>) to <jats:inline-formula> <jats:tex-math> <?CDATA ${N}_{{{\rm{H}}}_{2}}$?> </jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msub> <mml:mrow> <mml:mi>N</mml:mi> </mml:mrow> <mml:mrow> <mml:msub> <mml:mrow> <mml:mi mathvariant="normal">H</mml:mi> </mml:mrow> <mml:mrow> <mml:mn>2</mml:mn> </mml:mrow> </mml:msub> </mml:mrow> </mml:msub> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjsac063dieqn5.gif" xlink:type="simple" /> </jats:inline-formula>, the <jats:italic>X</jats:italic> <jats:sub>CO</jats:sub> factor, varies as a broken power law in <jats:inline-formula> <jats:tex-math> <?CDATA ${I}_{{}^{12}{\rm{CO}}}$?> </jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msub> <mml:mrow> <mml:mi>I</mml:mi> </mml:mrow> <mml:mrow> <mml:msup> <mml:mrow /> <mml:mrow> <mml:mn>12</mml:mn> </mml:mrow> </mml:msup> <mml:mi mathvariant="normal">CO</mml:mi> </mml:mrow> </mml:msub> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjsac063dieqn6.gif" xlink:type="simple" /> </jats:inline-formula> with a transition zone between 70 and 90 K km s<jats:sup>−1</jats:sup>. The <jats:italic>X</jats:italic> <jats:sub>CO</jats:sub> function we propose has <jats:inline-formula> <jats:tex-math> <?CDATA ${N}_{{{\rm{H}}}_{2}}\propto {I}_{{}^{12}{\rm{CO}}}^{0.51}$?> </jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msub> <mml:mrow> <mml:mi>N</mml:mi> </mml:mrow> <mml:mrow> <mml:msub> <mml:mrow> <mml:mi mathvariant="normal">H</mml:mi> </mml:mrow> <mml:mrow> <mml:mn>2</mml:mn> </mml:mrow> </mml:msub> </mml:mrow> </mml:msub> <mml:mo>∝</mml:mo> <mml:msubsup> <mml:mrow> <mml:mi>I</mml:mi> </mml:mrow> <mml:mrow> <mml:msup> <mml:mrow /> <mml:mrow> <mml:mn>12</mml:mn> </mml:mrow> </mml:msup> <mml:mi mathvariant="normal">CO</mml:mi> </mml:mrow> <mml:mrow> <mml:mn>0.51</mml:mn> </mml:mrow> </mml:msubsup> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjsac063dieqn7.gif" xlink:type="simple" /> </jats:inline-formula> for <jats:inline-formula> <jats:tex-math> <?CDATA ${I}_{{}^{12}{\rm{CO}}}\lesssim 70$?> </jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msub> <mml:mrow> <mml:mi>I</mml:mi> </mml:mrow> <mml:mrow> <mml:msup> <mml:mrow /> <mml:mrow> <mml:mn>12</mml:mn> </mml:mrow> </mml:msup> <mml:mi mathvariant="normal">CO</mml:mi> </mml:mrow> </mml:msub> <mml:mo>≲</mml:mo> <mml:mn>70</mml:mn> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjsac063dieqn8.gif" xlink:type="simple" /> </jats:inline-formula> K km s<jats:sup>−1</jats:sup> and <jats:inline-formula> <jats:tex-math> <?CDATA ${N}_{{{\rm{H}}}_{2}}\propto {I}_{{}^{12}{\rm{CO}}}^{2.3}$?> </jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msub> <mml:mrow> <mml:mi>N</mml:mi> </mml:mrow> <mml:mrow> <mml:msub> <mml:mrow> <mml:mi mathvariant="normal">H</mml:mi> </mml:mrow> <mml:mrow> <mml:mn>2</mml:mn> </mml:mrow> </mml:msub> </mml:mrow> </mml:msub> <mml:mo>∝</mml:mo> <mml:msubsup> <mml:mrow> <mml:mi>I</mml:mi> </mml:mrow> <mml:mrow> <mml:msup> <mml:mrow /> <mml:mrow> <mml:mn>12</mml:mn> </mml:mrow> </mml:msup> <mml:mi mathvariant="normal">CO</mml:mi> </mml:mrow> <mml:mrow> <mml:mn>2.3</mml:mn> </mml:mrow> </mml:msubsup> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjsac063dieqn9.gif" xlink:type="simple" /> </jats:inline-formula> for <jats:inline-formula> <jats:tex-math> <?CDATA ${I}_{{}^{12}{\rm{CO}}}\gtrsim 90$?> </jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msub> <mml:mrow> <mml:mi>I</mml:mi> </mml:mrow> <mml:mrow> <mml:msup> <mml:mrow /> <mml:mrow> <mml:mn>12</mml:mn> </mml:mrow> </mml:msup> <mml:mi mathvariant="normal">CO</mml:mi> </mml:mrow> </mml:msub> <mml:mo>≳</mml:mo> <mml:mn>90</mml:mn> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjsac063dieqn10.gif" xlink:type="simple" /> </jats:inline-formula> K km s<jats:sup>−1</jats:sup>. The high-<jats:inline-formula> <jats:tex-math> <?CDATA ${I}_{{}^{12}{\rm{CO}}}$?> </jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msub> <mml:mrow> <mml:mi>I</mml:mi> </mml:mrow> <mml:mrow> <mml:msup> <mml:mrow /> <mml:mrow> <mml:mn>12</mml:mn> </mml:mrow> </mml:msup> <mml:mi mathvariant="normal">CO</mml:mi> </mml:mrow> </mml:msub> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjsac063dieqn11.gif" xlink:type="simple" /> </jats:inline-formula> side should be generalizable with known adjustments for metallicity, but the influence of interstellar UV fields on the low-<jats:inline-formula> <jats:tex-math> <?CDATA ${I}_{{}^{12}{\rm{CO}}}$?> </jats:tex-math> <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msub> <mml:mrow> <mml:mi>I</mml:mi> </mml:mrow> <mml:mrow> <mml:msup> <mml:mrow /> <mml:mrow> <mml:mn>12</mml:mn> </mml:mrow> </mml:msup> <mml:mi mathvariant="normal">CO</mml:mi> </mml:mrow> </mml:msub> </mml:math> <jats:inline-graphic xmlns:xlink="http://www.w3.org/1999/xlink" xlink:href="apjsac063dieqn12.gif" xlink:type="simple" /> </jats:inline-formula> side may be sample specific. We discuss how these results expand on previous works in the CHaMP series and help tie together observational, theoretical, and laboratory studies on CO over the past decade.</jats:p>

<jats:title>Abstract</jats:title> <jats:p>We present redshifts for 2753 low-redshift galaxies between 0.03 ≲ <jats:italic>z</jats:italic> <jats:sub>spec</jats:sub> ≲ 0.5 with 18 ≤ <jats:italic>r</jats:italic> ≤ 22 obtained with Hectospec at the Multi-Mirror Telescope. The observations targeted the XMM-LSS, ELAIS-N1 and DEEP2-3 fields, each of which covers ∼1 deg<jats:sup>2</jats:sup>. These fields are also part of the recently completed Canada–France–Hawaii Telescope Large Area <jats:italic>U</jats:italic>-band Deep Survey and ongoing Hyper Suprime-Cam deep fields surveys. The efficiency of our technique for selecting low-redshift galaxies is confirmed by the redshift distribution of our sources. In addition to redshifts, these high signal-to-noise ratio spectra are used to measure ages, metallicities, and nuclear activity levels. In combination with the photometric catalog in <jats:italic>u</jats:italic>, <jats:italic>g</jats:italic>, <jats:italic>r</jats:italic>, <jats:italic>i</jats:italic>, <jats:italic>z</jats:italic>, <jats:italic>y</jats:italic> down to 27 AB mag, we are able to study the galaxy population down to stellar masses of ∼10<jats:sup>8</jats:sup> <jats:italic> M</jats:italic> <jats:sub>⊙</jats:sub>. This paper presents the observational strategy, the reduction procedure and properties of the galaxy sample. (The catalog can be accessed through the survey’s website at <jats:ext-link xmlns:xlink="http://www.w3.org/1999/xlink" ext-link-type="uri" xlink:href="http://mips.as.arizona.edu/~cnaw/Faint_Low_z/" xlink:type="simple">http://mips.as.arizona.edu/~cnaw/Faint_Low_z/</jats:ext-link>.)</jats:p>

<jats:title>Abstract</jats:title> <jats:p>The Complete Calibration of the Color–Redshift Relation (C3R2) survey is obtaining spectroscopic redshifts in order to map the relation between galaxy color and redshift to a depth of <jats:italic>i</jats:italic> ∼ 24.5 (AB). The primary goal is to enable sufficiently accurate photometric redshifts for Stage <jats:sc>iv</jats:sc> dark energy projects, particularly Euclid and the Nancy Grace Roman Space Telescope (Roman), which are designed to constrain cosmological parameters through weak lensing. We present 676 new high-confidence spectroscopic redshifts obtained by the C3R2 survey in the 2017B–2019B semesters using the DEIMOS, LRIS, and MOSFIRE multiobject spectrographs on the Keck telescopes. Combined with the 4454 redshifts previously published by this project, the C3R2 survey has now obtained and published 5130 high-quality galaxy spectra and redshifts. If we restrict consideration to only the 0.2 &lt; <jats:italic>z</jats:italic> <jats:sub> <jats:italic>p</jats:italic> </jats:sub> &lt; 2.6 range of interest for the Euclid cosmological goals, then with the current data release, C3R2 has increased the spectroscopic redshift coverage of the Euclid color space from 51% (as reported by Masters et al.) to the current 91%. Once completed and combined with extensive data collected by other spectroscopic surveys, C3R2 should provide the spectroscopic calibration set needed to enable photometric redshifts to meet the cosmology requirements for Euclid, and make significant headway toward solving the problem for Roman.</jats:p>