adsabs/AstroCLIMB huggingface dataset:
Paper: COSMOS2020: A Panchromatic View of the Universe to z ∼ 10 from Two Complementary Catalogs
Authors: J. R. Weaver, O. B. Kauffmann, O. Ilbert, H. J. McCracken, A. Moneti, S. Toft, G. Brammer, M. Shuntov, I. Davidzon, B. C. Hsieh, C. Laigle, A. Anastasiou, C. K. Jespersen, J. Vinther, P. Capak, C. M. Casey, C. J. R. McPartland, B. Milvang-Jensen, B. Mobasher, D. B. Sanders, L. Zalesky, S. Arnouts, H. Aussel, J. S. Dunlop, A. Faisst, M. Franx, L. J. Furtak, J. P. U. Fynbo, K. M. L. Gould, T. R. Greve, S. Gwyn, J. S. Kartaltepe, D. Kashino, A. M. Koekemoer, V. Kokorev, O. Le Fèvre, S. Lilly, D. Masters, G. Magdis, V. Mehta, Y. Peng, D. A. Riechers, M. Salvato, M. Sawicki, C. Scarlata, N. Scoville, R. Shirley, A. Sneppen, V. Smolc̆ić, C. Steinhardt, D. Stern, M. Tanaka, Y. Taniguchi, H. I. Teplitz, M. Vaccari, W.-H. Wang, and G. Zamorani
Figure caption: i- and Ks-band galaxy number counts of the izYJHKs-detected galaxies in the UltraVISTA ultradeep and deep regions, compared to a selection of literature measurements, including previous COSMOS catalogs. The bins follow increments of 0.5 mag, with the exception of Fontana et al. (2014), who use 0.25 mag.
Paper: COSMOS2020: A Panchromatic View of the Universe to z ∼ 10 from Two Complementary Catalogs
Authors: J. R. Weaver, O. B. Kauffmann, O. Ilbert, H. J. McCracken, A. Moneti, S. Toft, G. Brammer, M. Shuntov, I. Davidzon, B. C. Hsieh, C. Laigle, A. Anastasiou, C. K. Jespersen, J. Vinther, P. Capak, C. M. Casey, C. J. R. McPartland, B. Milvang-Jensen, B. Mobasher, D. B. Sanders, L. Zalesky, S. Arnouts, H. Aussel, J. S. Dunlop, A. Faisst, M. Franx, L. J. Furtak, J. P. U. Fynbo, K. M. L. Gould, T. R. Greve, S. Gwyn, J. S. Kartaltepe, D. Kashino, A. M. Koekemoer, V. Kokorev, O. Le Fèvre, S. Lilly, D. Masters, G. Magdis, V. Mehta, Y. Peng, D. A. Riechers, M. Salvato, M. Sawicki, C. Scarlata, N. Scoville, R. Shirley, A. Sneppen, V. Smolc̆ić, C. Steinhardt, D. Stern, M. Tanaka, Y. Taniguchi, H. I. Teplitz, M. Vaccari, W.-H. Wang, and G. Zamorani
Figure caption: Color–color diagrams showing stars (black) and galaxies (colored by zphot) classified by LePhare for THE FARMER photometry, shown in gzKs (top) and gzch1 (bottom) color–color diagrams. For simplicity, galaxies with zphot > 5 are shown also by red points. Only sources with S/N > 3 in g, z, Ks,  and  ch1 in the UltraVISTA area outside the HSC bright-star halos are shown.
Paper: COSMOS2020: A Panchromatic View of the Universe to z ∼ 10 from Two Complementary Catalogs
Authors: J. R. Weaver, O. B. Kauffmann, O. Ilbert, H. J. McCracken, A. Moneti, S. Toft, G. Brammer, M. Shuntov, I. Davidzon, B. C. Hsieh, C. Laigle, A. Anastasiou, C. K. Jespersen, J. Vinther, P. Capak, C. M. Casey, C. J. R. McPartland, B. Milvang-Jensen, B. Mobasher, D. B. Sanders, L. Zalesky, S. Arnouts, H. Aussel, J. S. Dunlop, A. Faisst, M. Franx, L. J. Furtak, J. P. U. Fynbo, K. M. L. Gould, T. R. Greve, S. Gwyn, J. S. Kartaltepe, D. Kashino, A. M. Koekemoer, V. Kokorev, O. Le Fèvre, S. Lilly, D. Masters, G. Magdis, V. Mehta, Y. Peng, D. A. Riechers, M. Salvato, M. Sawicki, C. Scarlata, N. Scoville, R. Shirley, A. Sneppen, V. Smolc̆ić, C. Steinhardt, D. Stern, M. Tanaka, Y. Taniguchi, H. I. Teplitz, M. Vaccari, W.-H. Wang, and G. Zamorani
Figure caption: Photometric redshifts computed with LePhare and EAZY, split by apparent magnitude bin (from i < 22.5 on the left to 25 < i < 27 on the right). Top: photo-z versus spec-z for the CLASSIC and THE FARMER photometric catalogs computed with LePhare. Bottom: photo-z versus spec-z for the CLASSIC and THE FARMER photometric catalogs computed with EAZY. The red solid line corresponds to the one-to-one relation, and the dashed lines correspond to the photo-z at ±0.15 (1 + zspec). The fraction of sources outside the dashed lines (noted η), the precision measured with the normalized absolute deviation (noted σ), and the overall bias (noted b) are indicated in each panel. The nature of the off-diagonal points, shown individually, are discussed in the text. Bin color increases on a log10 scale. The spec-z of i > 26 comprise 18% of sources shown in the rightmost 25 < i < 27 panels.
Paper: COSMOS2020: A Panchromatic View of the Universe to z ∼ 10 from Two Complementary Catalogs
Authors: J. R. Weaver, O. B. Kauffmann, O. Ilbert, H. J. McCracken, A. Moneti, S. Toft, G. Brammer, M. Shuntov, I. Davidzon, B. C. Hsieh, C. Laigle, A. Anastasiou, C. K. Jespersen, J. Vinther, P. Capak, C. M. Casey, C. J. R. McPartland, B. Milvang-Jensen, B. Mobasher, D. B. Sanders, L. Zalesky, S. Arnouts, H. Aussel, J. S. Dunlop, A. Faisst, M. Franx, L. J. Furtak, J. P. U. Fynbo, K. M. L. Gould, T. R. Greve, S. Gwyn, J. S. Kartaltepe, D. Kashino, A. M. Koekemoer, V. Kokorev, O. Le Fèvre, S. Lilly, D. Masters, G. Magdis, V. Mehta, Y. Peng, D. A. Riechers, M. Salvato, M. Sawicki, C. Scarlata, N. Scoville, R. Shirley, A. Sneppen, V. Smolc̆ić, C. Steinhardt, D. Stern, M. Tanaka, Y. Taniguchi, H. I. Teplitz, M. Vaccari, W.-H. Wang, and G. Zamorani
Figure caption: Photometric redshifts computed with LePhare and EAZY for the CLASSIC and THE FARMER photometric catalogs, split by apparent magnitude bin (from i < 22.5 on the left to 25 < i < 27 on the right). Top: comparison between the photometric redshifts computed with LePhare and EAZY for the full THE FARMER photometric catalog. Bottom: Comparison between the photo-z derived from the CLASSIC and THE FARMER full catalogs computed with LePhare (excluding masked regions). The nature of the two groups of off-diagonal points is discussed in the text. Bin color increases on a log10 scale. Note that the magnitude bins are different than in Figure 13 to illustrate the behavior at faint magnitudes.
Paper: COSMOS2020: A Panchromatic View of the Universe to z ∼ 10 from Two Complementary Catalogs
Authors: J. R. Weaver, O. B. Kauffmann, O. Ilbert, H. J. McCracken, A. Moneti, S. Toft, G. Brammer, M. Shuntov, I. Davidzon, B. C. Hsieh, C. Laigle, A. Anastasiou, C. K. Jespersen, J. Vinther, P. Capak, C. M. Casey, C. J. R. McPartland, B. Milvang-Jensen, B. Mobasher, D. B. Sanders, L. Zalesky, S. Arnouts, H. Aussel, J. S. Dunlop, A. Faisst, M. Franx, L. J. Furtak, J. P. U. Fynbo, K. M. L. Gould, T. R. Greve, S. Gwyn, J. S. Kartaltepe, D. Kashino, A. M. Koekemoer, V. Kokorev, O. Le Fèvre, S. Lilly, D. Masters, G. Magdis, V. Mehta, Y. Peng, D. A. Riechers, M. Salvato, M. Sawicki, C. Scarlata, N. Scoville, R. Shirley, A. Sneppen, V. Smolc̆ić, C. Steinhardt, D. Stern, M. Tanaka, Y. Taniguchi, H. I. Teplitz, M. Vaccari, W.-H. Wang, and G. Zamorani
Figure caption: Comparison between the precision (σNMAD) and the outlier fraction for the two catalogs (the CLASSIC in blue and THE FARMER in red) and for the two photo-z codes (LePhare with circles and EAZY with stars). The statistics are computed per i-band apparent magnitude bin, as indicated on the side of the points.
Paper: COSMOS2020: A Panchromatic View of the Universe to z ∼ 10 from Two Complementary Catalogs
Authors: J. R. Weaver, O. B. Kauffmann, O. Ilbert, H. J. McCracken, A. Moneti, S. Toft, G. Brammer, M. Shuntov, I. Davidzon, B. C. Hsieh, C. Laigle, A. Anastasiou, C. K. Jespersen, J. Vinther, P. Capak, C. M. Casey, C. J. R. McPartland, B. Milvang-Jensen, B. Mobasher, D. B. Sanders, L. Zalesky, S. Arnouts, H. Aussel, J. S. Dunlop, A. Faisst, M. Franx, L. J. Furtak, J. P. U. Fynbo, K. M. L. Gould, T. R. Greve, S. Gwyn, J. S. Kartaltepe, D. Kashino, A. M. Koekemoer, V. Kokorev, O. Le Fèvre, S. Lilly, D. Masters, G. Magdis, V. Mehta, Y. Peng, D. A. Riechers, M. Salvato, M. Sawicki, C. Scarlata, N. Scoville, R. Shirley, A. Sneppen, V. Smolc̆ić, C. Steinhardt, D. Stern, M. Tanaka, Y. Taniguchi, H. I. Teplitz, M. Vaccari, W.-H. Wang, and G. Zamorani
Figure caption: Cumulative distribution of the ratio between ∣zphot − zspec∣ and the photo-z 1σ uncertainty for both photometric catalogs and using LePhare. The photo-z 1σ uncertainty is taken as the maximum between ﹩({z}_{\mathrm{phot}}-{z}_{\mathrm{phot}}^{\min })﹩ and ﹩({z}_{\mathrm{phot}}^{\max }-{z}_{\mathrm{phot}})﹩. The solid and dashed lines correspond to the uncertainties from the CLASSIC and THE FARMER catalogs, respectively. For an unbiased estimate of the photo-z 1σ uncertainties, the cumulative number should reach 0.68 when the ratio equals 1 (black dotted line). The distributions are shown per bin of i-band magnitude.
Paper: COSMOS2020: A Panchromatic View of the Universe to z ∼ 10 from Two Complementary Catalogs
Authors: J. R. Weaver, O. B. Kauffmann, O. Ilbert, H. J. McCracken, A. Moneti, S. Toft, G. Brammer, M. Shuntov, I. Davidzon, B. C. Hsieh, C. Laigle, A. Anastasiou, C. K. Jespersen, J. Vinther, P. Capak, C. M. Casey, C. J. R. McPartland, B. Milvang-Jensen, B. Mobasher, D. B. Sanders, L. Zalesky, S. Arnouts, H. Aussel, J. S. Dunlop, A. Faisst, M. Franx, L. J. Furtak, J. P. U. Fynbo, K. M. L. Gould, T. R. Greve, S. Gwyn, J. S. Kartaltepe, D. Kashino, A. M. Koekemoer, V. Kokorev, O. Le Fèvre, S. Lilly, D. Masters, G. Magdis, V. Mehta, Y. Peng, D. A. Riechers, M. Salvato, M. Sawicki, C. Scarlata, N. Scoville, R. Shirley, A. Sneppen, V. Smolc̆ić, C. Steinhardt, D. Stern, M. Tanaka, Y. Taniguchi, H. I. Teplitz, M. Vaccari, W.-H. Wang, and G. Zamorani
Figure caption: Median of the photo-z 1σ uncertainties (defined as in Section 5.3) shown as a function of redshift. The shaded areas correspond to the COSMOS2020 CLASSIC catalog computed with LePhare, and the dashed lines correspond to the COSMOS2015 catalog. The distributions are shown per bin of i-band magnitude.
Paper: COSMOS2020: A Panchromatic View of the Universe to z ∼ 10 from Two Complementary Catalogs
Authors: J. R. Weaver, O. B. Kauffmann, O. Ilbert, H. J. McCracken, A. Moneti, S. Toft, G. Brammer, M. Shuntov, I. Davidzon, B. C. Hsieh, C. Laigle, A. Anastasiou, C. K. Jespersen, J. Vinther, P. Capak, C. M. Casey, C. J. R. McPartland, B. Milvang-Jensen, B. Mobasher, D. B. Sanders, L. Zalesky, S. Arnouts, H. Aussel, J. S. Dunlop, A. Faisst, M. Franx, L. J. Furtak, J. P. U. Fynbo, K. M. L. Gould, T. R. Greve, S. Gwyn, J. S. Kartaltepe, D. Kashino, A. M. Koekemoer, V. Kokorev, O. Le Fèvre, S. Lilly, D. Masters, G. Magdis, V. Mehta, Y. Peng, D. A. Riechers, M. Salvato, M. Sawicki, C. Scarlata, N. Scoville, R. Shirley, A. Sneppen, V. Smolc̆ić, C. Steinhardt, D. Stern, M. Tanaka, Y. Taniguchi, H. I. Teplitz, M. Vaccari, W.-H. Wang, and G. Zamorani
Figure caption: Redshift distribution for the CLASSIC (blue) and THE FARMER (red) full catalogs computed with LePhare. Each panel corresponds to a different magnitude limit in H band from THE FARMER.
Paper: COSMOS2020: A Panchromatic View of the Universe to z ∼ 10 from Two Complementary Catalogs
Authors: J. R. Weaver, O. B. Kauffmann, O. Ilbert, H. J. McCracken, A. Moneti, S. Toft, G. Brammer, M. Shuntov, I. Davidzon, B. C. Hsieh, C. Laigle, A. Anastasiou, C. K. Jespersen, J. Vinther, P. Capak, C. M. Casey, C. J. R. McPartland, B. Milvang-Jensen, B. Mobasher, D. B. Sanders, L. Zalesky, S. Arnouts, H. Aussel, J. S. Dunlop, A. Faisst, M. Franx, L. J. Furtak, J. P. U. Fynbo, K. M. L. Gould, T. R. Greve, S. Gwyn, J. S. Kartaltepe, D. Kashino, A. M. Koekemoer, V. Kokorev, O. Le Fèvre, S. Lilly, D. Masters, G. Magdis, V. Mehta, Y. Peng, D. A. Riechers, M. Salvato, M. Sawicki, C. Scarlata, N. Scoville, R. Shirley, A. Sneppen, V. Smolc̆ić, C. Steinhardt, D. Stern, M. Tanaka, Y. Taniguchi, H. I. Teplitz, M. Vaccari, W.-H. Wang, and G. Zamorani
Figure caption: Identification of quiescent galaxies in bins of redshift by selection in rest-frame NUV − r and r − J colors using the LePhare results, computed with THE FARMER for sources that lie above their respective mass-completeness limit. The selection is made using the prescription of Ilbert et al. (2013), shown in orange. For clarity, quiescent galaxies at z > 2.25 are shown by individual red points. r − J colors are highly uncertain at z > 2.6 where the rest-frame J band is extrapolated redward of the available photometry and hence have an uncertain classification marked by an orange dashed line.
Paper: COSMOS2020: A Panchromatic View of the Universe to z ∼ 10 from Two Complementary Catalogs
Authors: J. R. Weaver, O. B. Kauffmann, O. Ilbert, H. J. McCracken, A. Moneti, S. Toft, G. Brammer, M. Shuntov, I. Davidzon, B. C. Hsieh, C. Laigle, A. Anastasiou, C. K. Jespersen, J. Vinther, P. Capak, C. M. Casey, C. J. R. McPartland, B. Milvang-Jensen, B. Mobasher, D. B. Sanders, L. Zalesky, S. Arnouts, H. Aussel, J. S. Dunlop, A. Faisst, M. Franx, L. J. Furtak, J. P. U. Fynbo, K. M. L. Gould, T. R. Greve, S. Gwyn, J. S. Kartaltepe, D. Kashino, A. M. Koekemoer, V. Kokorev, O. Le Fèvre, S. Lilly, D. Masters, G. Magdis, V. Mehta, Y. Peng, D. A. Riechers, M. Salvato, M. Sawicki, C. Scarlata, N. Scoville, R. Shirley, A. Sneppen, V. Smolc̆ić, C. Steinhardt, D. Stern, M. Tanaka, Y. Taniguchi, H. I. Teplitz, M. Vaccari, W.-H. Wang, and G. Zamorani
Figure caption: Mass completeness for the total sample (yellow), as well as the star-forming (blue) and quiescent (red) populations using quantities derived from THE FARMER and LePhare considering magnitude limits of IRAC channel 1. Limits are calculated based on the method introduced in Pozzetti et al. (2010) in a manner consistent with COSMOS2015 (Davidzon et al. 2017, yellow dashed). For clarity, the total sample limit has been raised by 0.02 dex so that both it and the star-forming limit are visible.
Paper: COSMOS2020: A Panchromatic View of the Universe to z ∼ 10 from Two Complementary Catalogs
Authors: J. R. Weaver, O. B. Kauffmann, O. Ilbert, H. J. McCracken, A. Moneti, S. Toft, G. Brammer, M. Shuntov, I. Davidzon, B. C. Hsieh, C. Laigle, A. Anastasiou, C. K. Jespersen, J. Vinther, P. Capak, C. M. Casey, C. J. R. McPartland, B. Milvang-Jensen, B. Mobasher, D. B. Sanders, L. Zalesky, S. Arnouts, H. Aussel, J. S. Dunlop, A. Faisst, M. Franx, L. J. Furtak, J. P. U. Fynbo, K. M. L. Gould, T. R. Greve, S. Gwyn, J. S. Kartaltepe, D. Kashino, A. M. Koekemoer, V. Kokorev, O. Le Fèvre, S. Lilly, D. Masters, G. Magdis, V. Mehta, Y. Peng, D. A. Riechers, M. Salvato, M. Sawicki, C. Scarlata, N. Scoville, R. Shirley, A. Sneppen, V. Smolc̆ić, C. Steinhardt, D. Stern, M. Tanaka, Y. Taniguchi, H. I. Teplitz, M. Vaccari, W.-H. Wang, and G. Zamorani
Figure caption: Comparison of broadband Ks and IRAC channel 1 magnitudes and color between the THE FARMER catalog of this work with those of CANDELS (Nayyeri et al. 2017) and COSMOS2015 (Laigle et al. 2016). Individual sources are shown by the underlying density histogram that is described by the overlaid median binned by 0.2 AB with an envelope containing 68% of sources per bin. For the magnitudes, depths are shown for the comparison sample (dashed) and for COSMOS2020 (dotted), corresponding to 3σ depths measured with 3″ diameter apertures. For colors, averaged 3σ depth computed from both bands of interest measured with 3″ diameter apertures. The median Δmag offsets are reported for sources below the dashed magnitude limit.
Paper: The PHANGS-HST Survey: Physics at High Angular Resolution in Nearby Galaxies with the Hubble Space Telescope
Authors: Janice C. Lee, Bradley C. Whitmore, David A. Thilker, Sinan Deger, Kirsten L. Larson, Leonardo Ubeda, Gagandeep S. Anand, Mederic Boquien, Rupali Chandar, Daniel A. Dale, Eric Emsellem, Adam K. Leroy, Erik Rosolowsky, Eva Schinnerer, Judy Schmidt, James Lilly, Jordan Turner, Schuyler Van Dyk, Richard L. White, Ashley T. Barnes, Francesco Belfiore, Frank Bigiel, Guillermo A. Blanc, Yixian Cao, Melanie Chevance, Enrico Congiu, Oleg V. Egorov, Simon C. O. Glover, Kathryn Grasha, Brent Groves, Jonathan D. Henshaw, Annie Hughes, Ralf S. Klessen, Eric Koch, Kathryn Kreckel, J. M. Diederik Kruijssen, Daizhong Liu, Laura A. Lopez, Ness Mayker, Sharon E. Meidt, Eric J. Murphy, Hsi-An Pan, Jérôme Pety, Miguel Querejeta, Alessandro Razza, Toshiki Saito, Patricia Sánchez-Blázquez, Francesco Santoro, Amy Sardone, Fabian Scheuermann, Andreas Schruba, Jiayi Sun, Antonio Usero, E. Watkins, and Thomas G. Williams
Figure caption: Upper left: coverage of the SFR–M* plane by galaxies in the parent PHANGS sample (N = 74; orange open and filled points) and those targeted for HST observations (N = 38; orange filled points). The PHANGS-HST subsample is representative of the d ≲ 20 Mpc massive galaxy population on the local star-forming main sequence, which contains the bulk of molecular gas and present-day star formation. Shown for context are: an SDSS local galaxy sample, which extends over a much larger volume to z ≲ 0.3 (grayscale; Salim et al. 2016); the HST LEGUS sample (blue; Calzetti et al. 2015b), which focuses on the nearest galaxies (d ≲ 11 Mpc) and includes a significant number of lower mass dwarfs; and luminous infrared galaxies within ∼350 Mpc from the GOALS sample (red; U et al. 2012). Upper right: distribution of distances of galaxies in the PHANGS parent sample and those selected for HST observations. All distances are provided in Table 1 and are taken from the compilation of Anand et al. (2020), with an update for one new TRGB distance derived from PHANGS-HST observations taken after the publication of that paper (see Section 3.2). Altogether, the PHANGS-HST V- and I-band parallel imaging have yielded eight TRGB measurements, which represent the best-available distances for those galaxies. Bottom panels: PHANGS-HST also provides coverage of a full range of specific SFRs, molecular gas surface densities, and spiral galaxy morphologies. Galaxies with MUSE IFU spectroscopy are indicated (N = 19) with crosses in the upper left and bottom plots. These 19 galaxies comprise the sample targeted by the PHANGS-JWST Cycle 1 Treasury program (see Section 6).
Paper: The PHANGS-HST Survey: Physics at High Angular Resolution in Nearby Galaxies with the Hubble Space Telescope
Authors: Janice C. Lee, Bradley C. Whitmore, David A. Thilker, Sinan Deger, Kirsten L. Larson, Leonardo Ubeda, Gagandeep S. Anand, Mederic Boquien, Rupali Chandar, Daniel A. Dale, Eric Emsellem, Adam K. Leroy, Erik Rosolowsky, Eva Schinnerer, Judy Schmidt, James Lilly, Jordan Turner, Schuyler Van Dyk, Richard L. White, Ashley T. Barnes, Francesco Belfiore, Frank Bigiel, Guillermo A. Blanc, Yixian Cao, Melanie Chevance, Enrico Congiu, Oleg V. Egorov, Simon C. O. Glover, Kathryn Grasha, Brent Groves, Jonathan D. Henshaw, Annie Hughes, Ralf S. Klessen, Eric Koch, Kathryn Kreckel, J. M. Diederik Kruijssen, Daizhong Liu, Laura A. Lopez, Ness Mayker, Sharon E. Meidt, Eric J. Murphy, Hsi-An Pan, Jérôme Pety, Miguel Querejeta, Alessandro Razza, Toshiki Saito, Patricia Sánchez-Blázquez, Francesco Santoro, Amy Sardone, Fabian Scheuermann, Andreas Schruba, Jiayi Sun, Antonio Usero, E. Watkins, and Thomas G. Williams
Figure caption: PHANGS-HST WFC3 UVIS footprints (162″ × 162″) overlaid on PHANGS CO(2–1) ALMA maps for six galaxies in our sample of 38, showing the enormous diversity of molecular gas content and morphology in present-day massive star-forming galaxies. CO maps are overlaid on wider field DSS imaging. Scale bars and galaxy distances are shown in the upper and lower right corners, respectively. Top: Targets showing decreasing molecular gas surface density and specific SFR, from left to right. Bottom: impact of dynamical features on the gas distribution; two examples showing differing responses of the gas to the influence of a bar (left, middle) and an example of a ring feature (right). Our WFC3/UVIS observations allow us to find and characterize young stellar clusters and associations over the same area covered by these detailed CO maps, to create the first combined atlas of clouds and clusters across a representative sample of massive main-sequence galaxies in the local universe.
Paper: The PHANGS-HST Survey: Physics at High Angular Resolution in Nearby Galaxies with the Hubble Space Telescope
Authors: Janice C. Lee, Bradley C. Whitmore, David A. Thilker, Sinan Deger, Kirsten L. Larson, Leonardo Ubeda, Gagandeep S. Anand, Mederic Boquien, Rupali Chandar, Daniel A. Dale, Eric Emsellem, Adam K. Leroy, Erik Rosolowsky, Eva Schinnerer, Judy Schmidt, James Lilly, Jordan Turner, Schuyler Van Dyk, Richard L. White, Ashley T. Barnes, Francesco Belfiore, Frank Bigiel, Guillermo A. Blanc, Yixian Cao, Melanie Chevance, Enrico Congiu, Oleg V. Egorov, Simon C. O. Glover, Kathryn Grasha, Brent Groves, Jonathan D. Henshaw, Annie Hughes, Ralf S. Klessen, Eric Koch, Kathryn Kreckel, J. M. Diederik Kruijssen, Daizhong Liu, Laura A. Lopez, Ness Mayker, Sharon E. Meidt, Eric J. Murphy, Hsi-An Pan, Jérôme Pety, Miguel Querejeta, Alessandro Razza, Toshiki Saito, Patricia Sánchez-Blázquez, Francesco Santoro, Amy Sardone, Fabian Scheuermann, Andreas Schruba, Jiayi Sun, Antonio Usero, E. Watkins, and Thomas G. Williams
Figure caption: Figures showing the overlap of the PHANGS-HST WFC3 UVIS (blue), ALMA (red), and MUSE (where available; cyan) observation footprints, overlaid on DSS imaging for the same six galaxies as in Figure 2. A larger field (20′×20′) is shown relative to Figure 2 to illustrate the placement of the HST ACS parallel pointing (dashed lines). The WFC3 UVIS field of view is 162″ × 162″ and the ACS field of view is 202″ × 202″. Such footprint maps for the full PHANGS-HST sample can be found at https://archive.stsci.edu/hlsp/phangs-hst/.
Paper: The PHANGS-HST Survey: Physics at High Angular Resolution in Nearby Galaxies with the Hubble Space Telescope
Authors: Janice C. Lee, Bradley C. Whitmore, David A. Thilker, Sinan Deger, Kirsten L. Larson, Leonardo Ubeda, Gagandeep S. Anand, Mederic Boquien, Rupali Chandar, Daniel A. Dale, Eric Emsellem, Adam K. Leroy, Erik Rosolowsky, Eva Schinnerer, Judy Schmidt, James Lilly, Jordan Turner, Schuyler Van Dyk, Richard L. White, Ashley T. Barnes, Francesco Belfiore, Frank Bigiel, Guillermo A. Blanc, Yixian Cao, Melanie Chevance, Enrico Congiu, Oleg V. Egorov, Simon C. O. Glover, Kathryn Grasha, Brent Groves, Jonathan D. Henshaw, Annie Hughes, Ralf S. Klessen, Eric Koch, Kathryn Kreckel, J. M. Diederik Kruijssen, Daizhong Liu, Laura A. Lopez, Ness Mayker, Sharon E. Meidt, Eric J. Murphy, Hsi-An Pan, Jérôme Pety, Miguel Querejeta, Alessandro Razza, Toshiki Saito, Patricia Sánchez-Blázquez, Francesco Santoro, Amy Sardone, Fabian Scheuermann, Andreas Schruba, Jiayi Sun, Antonio Usero, E. Watkins, and Thomas G. Williams
Figure caption: Color composites of PHANGS-HST imaging (Red: WFC3/UVIS F814W, green: WFC3/UVIS F555W, blue: WFC3/UVIS F438W+F336W+F275W), overlaid on DSS imaging for the same six galaxies as in Figures 2 and 3.
Paper: The PHANGS-HST Survey: Physics at High Angular Resolution in Nearby Galaxies with the Hubble Space Telescope
Authors: Janice C. Lee, Bradley C. Whitmore, David A. Thilker, Sinan Deger, Kirsten L. Larson, Leonardo Ubeda, Gagandeep S. Anand, Mederic Boquien, Rupali Chandar, Daniel A. Dale, Eric Emsellem, Adam K. Leroy, Erik Rosolowsky, Eva Schinnerer, Judy Schmidt, James Lilly, Jordan Turner, Schuyler Van Dyk, Richard L. White, Ashley T. Barnes, Francesco Belfiore, Frank Bigiel, Guillermo A. Blanc, Yixian Cao, Melanie Chevance, Enrico Congiu, Oleg V. Egorov, Simon C. O. Glover, Kathryn Grasha, Brent Groves, Jonathan D. Henshaw, Annie Hughes, Ralf S. Klessen, Eric Koch, Kathryn Kreckel, J. M. Diederik Kruijssen, Daizhong Liu, Laura A. Lopez, Ness Mayker, Sharon E. Meidt, Eric J. Murphy, Hsi-An Pan, Jérôme Pety, Miguel Querejeta, Alessandro Razza, Toshiki Saito, Patricia Sánchez-Blázquez, Francesco Santoro, Amy Sardone, Fabian Scheuermann, Andreas Schruba, Jiayi Sun, Antonio Usero, E. Watkins, and Thomas G. Williams
Figure caption: Flowchart illustrating the PHANGS-HST star cluster and multiscale stellar association catalog pipeline. The chart begins at the upper left corner with the acquisition of HST imaging and proceeds from left to right along the rows, which represent the major components of the pipeline, and concludes with the production of catalogs at the bottom right of the chart. Dashed lines indicate high-level science products for public release via MAST, CADC, and the PHANGS collaboration website https://sites.google.com/view/phangs/home. † indicates that the galaxy distance is used in this step.