adsabs/AstroCLIMB huggingface dataset:
Paper: A Decade of Linear and Circular Polarimetry with the POLISH2 Polarimeter
Authors: Sloane J. Wiktorowicz, Agnieszka Słowikowska, Larissa A. Nofi, Nicole Rider, Angie Wolfgang, Ninos Hermis, Daniel Jontof-Hutter, Amanda J. Bayless, Gary M. Cole, Kirk B. Crawford, Valeri V. Tsarev, Michael C. Owens, Ernest G. Jaramillo, Geoffrey A. Maul, James R. Graham, Maxwell A. Millar-Blanchaer, Kimberly Bott, Jon C. Mauerhan
Figure caption: Lick 3 m POLISH2 B-band measurements of the weakly polarized HR 4295 as it is occulted by the telescope dome. The telescope polarization is subtracted as discussed in Section 3.5.2. The dashed, vertical lines indicate when dome occultation begins to be apparent in Stokes q.
Paper: A Decade of Linear and Circular Polarimetry with the POLISH2 Polarimeter
Authors: Sloane J. Wiktorowicz, Agnieszka Słowikowska, Larissa A. Nofi, Nicole Rider, Angie Wolfgang, Ninos Hermis, Daniel Jontof-Hutter, Amanda J. Bayless, Gary M. Cole, Kirk B. Crawford, Valeri V. Tsarev, Michael C. Owens, Ernest G. Jaramillo, Geoffrey A. Maul, James R. Graham, Maxwell A. Millar-Blanchaer, Kimberly Bott, Jon C. Mauerhan
Figure caption: Comparison of the measured degree of polarization p for a sample of stars between POLISH2, Starphysics Observatory 0.35 m CGPOL (open stars), and the literature (Heiles 2000; filled circles). POLISH2 measurements were obtained at both the Lick 3 m and 1 m telescopes. CGPOL measurements of all stars are consistent with POLISH2, which validates POLISH2 results asserting the Heiles (2000) values to be inaccurate for HD 18537 and HD 97991 (large, filled stars).
Paper: A Decade of Linear and Circular Polarimetry with the POLISH2 Polarimeter
Authors: Sloane J. Wiktorowicz, Agnieszka Słowikowska, Larissa A. Nofi, Nicole Rider, Angie Wolfgang, Ninos Hermis, Daniel Jontof-Hutter, Amanda J. Bayless, Gary M. Cole, Kirk B. Crawford, Valeri V. Tsarev, Michael C. Owens, Ernest G. Jaramillo, Geoffrey A. Maul, James R. Graham, Maxwell A. Millar-Blanchaer, Kimberly Bott, Jon C. Mauerhan
Figure caption: Lick 1 m POLISH2 UBV measurements of telescope polarization from 2011 to 2014. The telescope polarization is typically p ∼ 500 ppm (0.05%) with an orientation of Θ ∼ 0° with respect to celestial north. The polarization data are rotated by the ﹩{\rm{\Theta }}^{\prime} \sim 151^\circ ﹩ rotational offset of the Lick 1 m Cassegrain ring (Section 3.2).
Paper: A Decade of Linear and Circular Polarimetry with the POLISH2 Polarimeter
Authors: Sloane J. Wiktorowicz, Agnieszka Słowikowska, Larissa A. Nofi, Nicole Rider, Angie Wolfgang, Ninos Hermis, Daniel Jontof-Hutter, Amanda J. Bayless, Gary M. Cole, Kirk B. Crawford, Valeri V. Tsarev, Michael C. Owens, Ernest G. Jaramillo, Geoffrey A. Maul, James R. Graham, Maxwell A. Millar-Blanchaer, Kimberly Bott, Jon C. Mauerhan
Figure caption: Same as Figure 13 but for Gemini North POLISH2 B-band measurements of the weakly polarized HR 8585. The telescope polarization is not subtracted, and its large, ∼0.3% value is manifested in the mean values of q, u, and p.
Paper:  12CO (3–2) High-Resolution Survey (COHRS) of the Galactic Plane: Complete Data Release
Authors: Geumsook Park, 금숙 박, Malcolm J. Currie, Holly S. Thomas, Erik Rosolowsky, Jessica T. Dempsey, Kee-Tae Kim, Andrew J. Rigby, Yang Su, David J. Eden, Dario Colombo, Harriet Parsons, Toby J. T. Moore
Figure caption: Integrated l distribution of 12CO (1–0) (FUGIN; black), 12CO (3–2) (COHRS; blue), Galactic H II regions (WISE; red in the top and bottom panels), star-forming clumps (ATLASGAL; orange in the middle and bottom panels), and the line ratio R 31 (gray and green in the bottom panel). Each profile is integrated over b ≤ 0.°5 and −60 km s−1 < v LSR < +170 km s−1. The star-forming clumps comprise all clumps except starless ones in the ATLASGAL compact-source catalog, that is, MSF clumps, YSO-forming clumps, and protostellar clumps. The CO histograms are drawn in the same way as in Figure 11, but are interpolated to have the same bin size (12′) and abscissa values as those of the H II regions and star-forming clumps. For the H II regions and star-forming clumps, each histogram was obtained by counting the number of sources in a moving bin with a population-counting bin width of 1° and a moving-bin interval of 12′. The green profile (R 31,2) is the ratio of the two CO transition profiles in the upper panels, but on an absolute scale that is not normalized by the maximum. Likewise, the gray profile (R 31,1) is the ratio on the absolute scale of the two CO profiles shown in Figure 11. Three vertical dotted lines are drawn to help locate three star-forming regions: W43 (l = 30.°8), W49A (43.°2), and W51 (49.°4).
Paper:  12CO (3–2) High-Resolution Survey (COHRS) of the Galactic Plane: Complete Data Release
Authors: Geumsook Park, 금숙 박, Malcolm J. Currie, Holly S. Thomas, Erik Rosolowsky, Jessica T. Dempsey, Kee-Tae Kim, Andrew J. Rigby, Yang Su, David J. Eden, Dario Colombo, Harriet Parsons, Toby J. T. Moore
Figure caption: Integrated (one-dimensional) l, b, and v LSR distributions of 12CO (1–0) (FUGIN; black) and 12CO (3–2) (COHRS; blue). Each profile was obtained by integrating across the two orthogonal axes. Note that the b- and v-profiles are restricted to data within 10° ≤ l ≤ 50° since available FUGIN data are limited to that Galactic longitudinal range. CO intensity was normalized to the peak value of each profile. The two CO l-profiles were smoothed to have a bin size of ∼60″, while the b- and v-profiles have a bin size corresponding to the latitudinal pixel size and velocity channel width of each CO data cube, respectively. On the top panel, three vertical dotted lines are drawn to help locate three star-forming regions: W43 (l = 30.°8), W49A (43.°2), and W51 (49.°4).
Paper:  12CO (3–2) High-Resolution Survey (COHRS) of the Galactic Plane: Complete Data Release
Authors: Geumsook Park, 금숙 박, Malcolm J. Currie, Holly S. Thomas, Erik Rosolowsky, Jessica T. Dempsey, Kee-Tae Kim, Andrew J. Rigby, Yang Su, David J. Eden, Dario Colombo, Harriet Parsons, Toby J. T. Moore
Figure caption: Scatterplots between two targets using the normalized histogram values shown in Figure 12: clockwise from top left, 12CO (1–0) vs. 12CO (3–2), WISE H II regions (red) or ATLASGAL star-forming clumps (orange) vs. R 31, star-forming clumps vs. CO emission, and WISE H II regions vs. CO emission. In the two bottom panels, 12CO (1–0) and 12CO (3–2) are displayed with black and blue circles, respectively. A solid line is the best result of a least-squares fit in a linear model using the IDL LINFIT procedure.
Paper:  12CO (3–2) High-Resolution Survey (COHRS) of the Galactic Plane: Complete Data Release
Authors: Geumsook Park, 금숙 박, Malcolm J. Currie, Holly S. Thomas, Erik Rosolowsky, Jessica T. Dempsey, Kee-Tae Kim, Andrew J. Rigby, Yang Su, David J. Eden, Dario Colombo, Harriet Parsons, Toby J. T. Moore
Figure caption: Position–velocity (l−v LSR) map for the 12CO (3–2) emission (T mb) in COHRS. This map was obtained by integrating over the latitude axis. The map is drawn on a square-root scale. The units on the intensity scale are K degrees. The bottom image is the same as the top, but is shown for a narrower velocity range overlaid with known H II regions and spiral arm loci. Cross symbols indicate WISE H II regions. The traces of the main spiral arms (Scutum Arm, Sagittarius Arm, Perseus Arm, and Norma-Outer Arm) and interarm features (Local Spur, Aquila Spur, Aquila Rift, and 3 kpc Arm) from Reid et al. (2016, 2019) are overlaid using black curves.
Paper:  12CO (3–2) High-Resolution Survey (COHRS) of the Galactic Plane: Complete Data Release
Authors: Geumsook Park, 금숙 박, Malcolm J. Currie, Holly S. Thomas, Erik Rosolowsky, Jessica T. Dempsey, Kee-Tae Kim, Andrew J. Rigby, Yang Su, David J. Eden, Dario Colombo, Harriet Parsons, Toby J. T. Moore
Figure caption: W43 star-forming region within the COHRS coverage area. From the top left to the bottom, each panel displays 12CO (1–0) FUGIN data, 12CO (3–2) COHRS data, 13CO (1–0) FUGIN data, 13CO (3–2) CHIMPS data, 8 μm GLIMPSE data, 850 μm JPS data, and examples of CO spectra, respectively. The CO maps are velocity-integrated over the v LSR range of (80, 110) km s−1 (Nguyen Luong et al. 2011), and the units on the intensity scale of the integrated main-beam temperature are K km s−1. The units on the intensity scale of the GLIMPSE and JPS data are MJy sr–1 and Jy beam–1, respectively. The CO spectra were obtained at the position closest to the velocity-integrated 12CO (3–2) emission peak. The offsets of 10 K, 20 K, and 30 K to the spectra have been added for better visualization.
Paper:  12CO (3–2) High-Resolution Survey (COHRS) of the Galactic Plane: Complete Data Release
Authors: Geumsook Park, 금숙 박, Malcolm J. Currie, Holly S. Thomas, Erik Rosolowsky, Jessica T. Dempsey, Kee-Tae Kim, Andrew J. Rigby, Yang Su, David J. Eden, Dario Colombo, Harriet Parsons, Toby J. T. Moore
Figure caption: Same as Figure 8, but for the W51 star-forming region. The CO maps are velocity-integrated over the v LSR range of (30, 85) km s−1 (Kang et al. 2010). There are no available CHIMPS data for this region.
Paper:  12CO (3–2) High-Resolution Survey (COHRS) of the Galactic Plane: Complete Data Release
Authors: Geumsook Park, 금숙 박, Malcolm J. Currie, Holly S. Thomas, Erik Rosolowsky, Jessica T. Dempsey, Kee-Tae Kim, Andrew J. Rigby, Yang Su, David J. Eden, Dario Colombo, Harriet Parsons, Toby J. T. Moore
Figure caption: Same as Figure 8, but for the W49A star-forming region. The 850 μm continuum data were taken from Eden et al. (2018). The CO maps are velocity-integrated over the v LSR range of (−20, +30) km s−1 (Galvan-Madrid et al. 2013). In the GLIMPSE 8 μm image, instrumental artifacts remain around the bright W49 area at (l, b) ∼ (43.°17, −0.°01).
Paper:  12CO (3–2) High-Resolution Survey (COHRS) of the Galactic Plane: Complete Data Release
Authors: Geumsook Park, 금숙 박, Malcolm J. Currie, Holly S. Thomas, Erik Rosolowsky, Jessica T. Dempsey, Kee-Tae Kim, Andrew J. Rigby, Yang Su, David J. Eden, Dario Colombo, Harriet Parsons, Toby J. T. Moore
Figure caption: Temperature PDFs of the entire 12CO (3–2) distribution (black) and the H II region–related 12CO (3–2) distribution (red) in COHRS.
Paper:  12CO (3–2) High-Resolution Survey (COHRS) of the Galactic Plane: Complete Data Release
Authors: Geumsook Park, 금숙 박, Malcolm J. Currie, Holly S. Thomas, Erik Rosolowsky, Jessica T. Dempsey, Kee-Tae Kim, Andrew J. Rigby, Yang Su, David J. Eden, Dario Colombo, Harriet Parsons, Toby J. T. Moore
Figure caption: Noise maps for the COHRS data. The noise level was obtained by the conventional way, which calculates rms values over velocity ranges where there is no astronomical signal (see text for details). The intensity scale is in ﹩{T}_{{\rm{A}}}^{* }﹩ (K).
Paper:  12CO (3–2) High-Resolution Survey (COHRS) of the Galactic Plane: Complete Data Release
Authors: Geumsook Park, 금숙 박, Malcolm J. Currie, Holly S. Thomas, Erik Rosolowsky, Jessica T. Dempsey, Kee-Tae Kim, Andrew J. Rigby, Yang Su, David J. Eden, Dario Colombo, Harriet Parsons, Toby J. T. Moore
Figure caption: Histogram of the S/N for all voxels in COHRS, displayed on a logarithmic scale. The bin width is 0.1 K. The blue curve is a Gaussian with a width (standard deviation) of 1 centered at 0. The inset shows the same distribution on a linear scale.
Paper:  12CO (3–2) High-Resolution Survey (COHRS) of the Galactic Plane: Complete Data Release
Authors: Geumsook Park, 금숙 박, Malcolm J. Currie, Holly S. Thomas, Erik Rosolowsky, Jessica T. Dempsey, Kee-Tae Kim, Andrew J. Rigby, Yang Su, David J. Eden, Dario Colombo, Harriet Parsons, Toby J. T. Moore
Figure caption: The maps of velocity-integrated emission (﹩{T}_{{\rm{A}}}^{* }﹩) in COHRS. These maps were obtained by integrating over the velocity range written at the top of each panel. The units on the intensity scale are K km s−1.
Paper: The JCMT SCUBA-2 Survey of the James Webb Space Telescope North Ecliptic Pole Time-Domain Field
Authors: Minhee Hyun, Myungshin Im, Ian R. Smail, William D. Cotton, Jack E. Birkin, Satoshi Kikuta, Hyunjin Shim, Christopher N. A. Willmer, James J. Condon, Rogier A. Windhorst, Seth H. Cohen, Rolf A. Jansen, Chun Ly, Yuichi Matsuda, Giovanni G. Fazio, A. M. Swinbank, Haojing Yan
Figure caption: Cumulative area as a function of sensitivity of the S2TDF (black solid line). The instrumental sensitivity of our map reaches σ inst = 0.8 mJy beam−1 in the deepest region of the field covering 0.087 deg2 and this is quite close to the confusion limit of SCUBA-2 850 μm, 0.7 mJy beam−1 (red dashed line). For comparison, the S2CLS EGS (blue dot; Zavala et al. 2017) covering 0.019 deg2 with a 1σ depth has σ inst = 0.46 mJy beam−1; the S2CLS GOODS-N (green asterisk; Geach et al. 2017) covering 0.07 deg2 with a 1σ depth has σ inst = 1.1 mJy beam−1; the SCUBA-2 survey in the COSMOS field (light green triangle; Casey et al. 2013) covering 0.109 deg2 with a 1σ depth has σ inst = 0.8 mJy beam−1; SUPER GOODS (pink cross; Cowie et al. 2017, 2018) covering 0.233 deg2 with a 1σ depth has σ inst = 1.8 mJy beam−1 and reaches σ inst = 0.4 mJy beam−1 in the deepest central field covering 0.018 deg2 (brown cross); the S2CLS NEP (purple diamond; Geach et al. 2017) covering 0.6 deg2 with a 1σ depth has σ inst = 1.2 mJy beam−1; the S2COSMOS (orange square; Simpson et al. 2019) covering 1.6 deg2 with a median noise level has σ inst = 1.2 mJy beam−1; and the NEPSC2 (yellow star; Shim et al. 2020) covering 2 deg2 with a median noise level has σ inst = 2.3 mJy beam−1. The horizontal cyan solid line shows the final area (r = 600″) of this work where we performed source detection (see Figure 3).
Paper: The JCMT SCUBA-2 Survey of the James Webb Space Telescope North Ecliptic Pole Time-Domain Field
Authors: Minhee Hyun, Myungshin Im, Ian R. Smail, William D. Cotton, Jack E. Birkin, Satoshi Kikuta, Hyunjin Shim, Christopher N. A. Willmer, James J. Condon, Rogier A. Windhorst, Seth H. Cohen, Rolf A. Jansen, Chun Ly, Yuichi Matsuda, Giovanni G. Fazio, A. M. Swinbank, Haojing Yan
Figure caption: The S/N map for the 41.3 hr of SCUBA-2 observations of the JWST-TDF. The cyan dashed circle is the area (r = 10′) where we performed source detection (σ inst< 1.5 mJy beam−1) and the noise levels (1.0, 1.5, 2.0, and 3.0 mJy) are indicated by white contours. In the deepest region of the field, the instrumental noise reaches 0.8 mJy beam−1, and the mean of σ inst is 1.0 mJy beam−1.
Paper: The JCMT SCUBA-2 Survey of the James Webb Space Telescope North Ecliptic Pole Time-Domain Field
Authors: Minhee Hyun, Myungshin Im, Ian R. Smail, William D. Cotton, Jack E. Birkin, Satoshi Kikuta, Hyunjin Shim, Christopher N. A. Willmer, James J. Condon, Rogier A. Windhorst, Seth H. Cohen, Rolf A. Jansen, Chun Ly, Yuichi Matsuda, Giovanni G. Fazio, A. M. Swinbank, Haojing Yan
Figure caption: SCUBA-2 flux map of JWST-TDF showing 83 detected sources at S/N > 4 and a further 31 with S/N = 3.5–4. The color of the sources represents their deboosted flux (see color bar) and thicker symbols represent S/N > 4 sources. By matching the 850 μm sources to the VLA 3 GHz catalog using a corrected Poissonian probability estimate, we found that 66 submm sources have radio counterparts (box symbols). Circle symbols are submm sources without radio identifications. The JWST NIRISS and NIRCam survey areas are indicated by dotted and dashed circles, respectively.
Paper: The JCMT SCUBA-2 Survey of the James Webb Space Telescope North Ecliptic Pole Time-Domain Field
Authors: Minhee Hyun, Myungshin Im, Ian R. Smail, William D. Cotton, Jack E. Birkin, Satoshi Kikuta, Hyunjin Shim, Christopher N. A. Willmer, James J. Condon, Rogier A. Windhorst, Seth H. Cohen, Rolf A. Jansen, Chun Ly, Yuichi Matsuda, Giovanni G. Fazio, A. M. Swinbank, Haojing Yan
Figure caption: The distribution of the JCMT-TDF SCUBA-2 observations undertaken in the 2018B, 2019B, and 2020X semesters. Colors represent the weather conditions of the observations, defined in “bands” calculated from the sky opacity, τ 225. The data for 2018B were obtained typically in better conditions than those in which the data for the 2019B and 2020X semesters were obtained. Each observation block (minimum schedulable block (MSB)) consists of an ∼40 minute exposure with the PONG900 scanning mode. The total exposure time is 41.3 hr (corresponding to 62 MSBs).
Paper: The JCMT SCUBA-2 Survey of the James Webb Space Telescope North Ecliptic Pole Time-Domain Field
Authors: Minhee Hyun, Myungshin Im, Ian R. Smail, William D. Cotton, Jack E. Birkin, Satoshi Kikuta, Hyunjin Shim, Christopher N. A. Willmer, James J. Condon, Rogier A. Windhorst, Seth H. Cohen, Rolf A. Jansen, Chun Ly, Yuichi Matsuda, Giovanni G. Fazio, A. M. Swinbank, Haojing Yan
Figure caption: Illustration of the multiwavelength data coverage in the JWST-TDF survey region. The inner dashed green and dotted dark blue circles are the NIRISS and NIRCam survey areas, respectively (10′ and 14′ diameters, respectively). The data coverage from other facilities is shown in different colors as indicated (for more details, see Jansen & Windhorst 2018). The solid blue circle represents the JCMT SCUBA-2 850 μm survey area analyzed in this work and the VLA 3 GHz observations, with a 24′ diameter field of view, cover the full field.
Paper: The JCMT SCUBA-2 Survey of the James Webb Space Telescope North Ecliptic Pole Time-Domain Field
Authors: Minhee Hyun, Myungshin Im, Ian R. Smail, William D. Cotton, Jack E. Birkin, Satoshi Kikuta, Hyunjin Shim, Christopher N. A. Willmer, James J. Condon, Rogier A. Windhorst, Seth H. Cohen, Rolf A. Jansen, Chun Ly, Yuichi Matsuda, Giovanni G. Fazio, A. M. Swinbank, Haojing Yan
Figure caption: In both panels, red and pink filled circles show the S2TDF sources at S/N > 4.0 and at S/N = 3.5–4.0, respectively. The median errors are also presented (green). (Top) The variation in cold dust mass from MAGPHYS for our SMGs with redshift. We compare this to that of a similarly radio-detected and K < 22.5 sample of SMGs from AS2UDS (Dudzevičiūtė et al. 2020). The details of the symbols are the same as those in Figure 12. In addition, we show a K-band-selected field galaxy sample with K < 22.5 (gray points) and the trend (yellow solid line) of estimated dust masses from Dudzevičiūtė et al. (2020). This illustrates significantly higher cold dust masses, and by implication higher cold gas masses, for the SMGs, compared to typical star-forming galaxies at similar redshifts. (Bottom) DSR as a function of redshift for radio-identified SMGs in this work and in AS2UDS (Dudzevičiūtė et al. 2020). For comparison we present the median DSR of various samples collated by Calura et al. (2017) with open diamond symbols: blue, cyan, deep pink, brown, and purple colors represent spiral galaxies from SINGS (Kennicutt et al. 2003), spiral galaxies from KINGFISH (Kennicutt et al. 2011), a local ULIRG sample (Clements et al. 2010), FIR-selected galaxies in the COSMOS/GOODS surveys (Calura et al. 2017; Lutz et al. 2011), and higher-redshift SMGs (Greve et al. 2005; Santini et al. 2010), respectively. We also show the model predictions of “main-sequence” and starburst dusty star-forming galaxies from Davé et al. (2019) and Pantoni et al. (2019), respectively.
Paper: The JCMT SCUBA-2 Survey of the James Webb Space Telescope North Ecliptic Pole Time-Domain Field
Authors: Minhee Hyun, Myungshin Im, Ian R. Smail, William D. Cotton, Jack E. Birkin, Satoshi Kikuta, Hyunjin Shim, Christopher N. A. Willmer, James J. Condon, Rogier A. Windhorst, Seth H. Cohen, Rolf A. Jansen, Chun Ly, Yuichi Matsuda, Giovanni G. Fazio, A. M. Swinbank, Haojing Yan
Figure caption: (a) Completeness of the JWST-TDF SCUBA-2 survey calculated from the ratio of the number of recovered sources with S/N > 3.5 to the number of input sources. The 50% and 80% completeness limits are 3.0 and 4.0 mJy (deboosted flux), respectively. (b) The false detection rate, the ratio between the number of sources detected in the jackknife map and that of sources detected in the flux density map (inner panel), as a function of S/N. With an S/N > 3.5 cut the probability that a detected source is spurious is ≃8%, and at S/N > 4 it is ≃1%; this drops to 0% at S/N > 4.25. (c) Average flux boosting factor as a function of S/N, showing that the results are well fitted with a power law. However, we evaluated boosting rates for each source based on the observed flux density and the local instrumental noise by constructing a two-dimensional parameter space. (d) The total positional error in both R.A. and decl. directions (solid line), which is the quadratic sum of the intrinsic positional error (σ 0, dashed line) and the positional difference with the bootstrapping error (σ, dotted line), as a function of S/N. Red filled circles are the standard deviation of the R.A. and decl. position offsets between the SCUBA-2 sources and their VLA counterparts.
Paper: The JCMT SCUBA-2 Survey of the James Webb Space Telescope North Ecliptic Pole Time-Domain Field
Authors: Minhee Hyun, Myungshin Im, Ian R. Smail, William D. Cotton, Jack E. Birkin, Satoshi Kikuta, Hyunjin Shim, Christopher N. A. Willmer, James J. Condon, Rogier A. Windhorst, Seth H. Cohen, Rolf A. Jansen, Chun Ly, Yuichi Matsuda, Giovanni G. Fazio, A. M. Swinbank, Haojing Yan
Figure caption: Photometric redshift vs. flux density and flux ratio for SCUBA-2 SMGs. S2TDF sources at S/N > 4.0 and at S/N = 3.5–4.0 are presented with filled red circles and with filled pink circles, respectively. The median error of each parameter is drawn in each panel (green). (Left) 850 μm flux density vs. photometric redshift for our radio-identified SMGs with optical/NIR counterparts. For comparison we show a radio and K-band limited subsample of SMGs from AS2UDS (Dudzevičiūtė et al. 2020), and the fitted trend for the full AS2UDS survey from Stach et al. (2019). There is broad agreement between the redshift–flux distributions in the JWST-TDF and these previous works. (Right) The variation in submm-to-radio flux ratio and photometric redshift for our sample, again compared to a radio/K-band-limited subset of the SMGs in AS2UDS (converted from 1.4 to 3 GHz assuming a radio spectral index of −0.7). We also show the expected trend for the composite SMG SED from Dudzevičiūtė et al. (2020), which broadly reproduces the behavior we see.
Paper: The JCMT SCUBA-2 Survey of the James Webb Space Telescope North Ecliptic Pole Time-Domain Field
Authors: Minhee Hyun, Myungshin Im, Ian R. Smail, William D. Cotton, Jack E. Birkin, Satoshi Kikuta, Hyunjin Shim, Christopher N. A. Willmer, James J. Condon, Rogier A. Windhorst, Seth H. Cohen, Rolf A. Jansen, Chun Ly, Yuichi Matsuda, Giovanni G. Fazio, A. M. Swinbank, Haojing Yan
Figure caption: SFR–M * distribution for the S2TDF, compared to a K < 22.5 limited, radio-selected subsample of SMGs from AS2UDS (Dudzevičiūtė et al. 2020). We show the median error at the bottom left corner in green. The solid line is the linear trend derived from a sample of K-band-detected field galaxies that has been matched to the S2TDF SMGs in redshift and stellar mass (see the main text), and the shaded area indicates the 20% uncertainty in the normalization. We also show the SFR–stellar mass relation for the “main sequence” of star-forming galaxies at various redshifts derived in Pearson et al. (2018). Both of these demonstrate that the S2TDF SMGs have SFRs above those typical for similar-mass field galaxies at their redshifts.