adsabs/AstroCLIMB huggingface dataset:
Paper:  pathfinder: A Semantic Framework for Literature Review and Knowledge Discovery in Astronomy
Authors: Kartheik G. Iyer, Mikaeel Yunus, Charles O'Neill, Christine Ye, Alina Hyk, Kiera McCormick, Ioana Ciucă, John F. Wu, Alberto Accomazzi, Simone Astarita, Rishabh Chakrabarty, Jesse Cranney, Anjalie Field, Tirthankar Ghosal, Michele Ginolfi, Marc Huertas-Company, Maja Jabłońska, Sandor Kruk, Huiling Liu, Gabriel Marchidan, Rohit Mistry, J. P. Naiman, J. E. G. Peek, Mugdha Polimera, Sergio J. Rodríguez Méndez, Kevin Schawinski, Sanjib Sharma, Michael J. Smith, Yuan-Sen Ting, Mike Walmsley
Figure caption: Example of pathfinder being asked a question, with explanations of the various toggles available to customize the output shown as numbered blue circles. Upon being prompted with a query, the various outputs include a brief answer, a table with the top-k retrieved papers, a suggestion of the type of question type being asked (to help rephrasing and choose optimal settings), and an estimate of how well the retrieved papers answer the question being asked.
Paper:  pathfinder: A Semantic Framework for Literature Review and Knowledge Discovery in Astronomy
Authors: Kartheik G. Iyer, Mikaeel Yunus, Charles O'Neill, Christine Ye, Alina Hyk, Kiera McCormick, Ioana Ciucă, John F. Wu, Alberto Accomazzi, Simone Astarita, Rishabh Chakrabarty, Jesse Cranney, Anjalie Field, Tirthankar Ghosal, Michele Ginolfi, Marc Huertas-Company, Maja Jabłońska, Sandor Kruk, Huiling Liu, Gabriel Marchidan, Rohit Mistry, J. P. Naiman, J. E. G. Peek, Mugdha Polimera, Sergio J. Rodríguez Méndez, Kevin Schawinski, Sanjib Sharma, Michael J. Smith, Yuan-Sen Ting, Mike Walmsley
Figure caption: Normalized single-document benchmark and multidocument benchmark scores across methods. Single-document scores consist of an average of reciprocal rank and success rate in retrieving the correct paper in the top 10 documents, normalized so the scores sum to 1. Similarly, the multidocument scores are an average of the normalized discounted cumulative gain (nDCG) at 100 documents and recall at 100 documents, again normalized. A combination of HYDE and reranking (HydeCohereRerank) was the best-performing system, outperforming HYDE alone, a base semantic search (with just the embeddings cosine similarity between query and documents), and a simple bag-of-words system.
Paper:  pathfinder: A Semantic Framework for Literature Review and Knowledge Discovery in Astronomy
Authors: Kartheik G. Iyer, Mikaeel Yunus, Charles O'Neill, Christine Ye, Alina Hyk, Kiera McCormick, Ioana Ciucă, John F. Wu, Alberto Accomazzi, Simone Astarita, Rishabh Chakrabarty, Jesse Cranney, Anjalie Field, Tirthankar Ghosal, Michele Ginolfi, Marc Huertas-Company, Maja Jabłońska, Sandor Kruk, Huiling Liu, Gabriel Marchidan, Rohit Mistry, J. P. Naiman, J. E. G. Peek, Mugdha Polimera, Sergio J. Rodríguez Méndez, Kevin Schawinski, Sanjib Sharma, Michael J. Smith, Yuan-Sen Ting, Mike Walmsley
Figure caption: Similar to Figure 2, but showing the loci of the top-level Unified Astronomy Thesaurus (UAT) hierarchical keywords projected into the embedding space. Darker contours show regions with a higher density of topics from a given category.
Paper:  pathfinder: A Semantic Framework for Literature Review and Knowledge Discovery in Astronomy
Authors: Kartheik G. Iyer, Mikaeel Yunus, Charles O'Neill, Christine Ye, Alina Hyk, Kiera McCormick, Ioana Ciucă, John F. Wu, Alberto Accomazzi, Simone Astarita, Rishabh Chakrabarty, Jesse Cranney, Anjalie Field, Tirthankar Ghosal, Michele Ginolfi, Marc Huertas-Company, Maja Jabłońska, Sandor Kruk, Huiling Liu, Gabriel Marchidan, Rohit Mistry, J. P. Naiman, J. E. G. Peek, Mugdha Polimera, Sergio J. Rodríguez Méndez, Kevin Schawinski, Sanjib Sharma, Michael J. Smith, Yuan-Sen Ting, Mike Walmsley
Figure caption: Annual Reviews in Astronomy and Astrophysics (ARA&A) articles shown in the space of astronomy papers. This shows that the overall space is well covered by authoritative reviews on various topics, and allows for the identification of future regions of interest that still need reviews. Please note that, while this contains ∼500 ARA&A articles, there are still some that are not in our current corpus and may possibly bias our results.
Paper:  pathfinder: A Semantic Framework for Literature Review and Knowledge Discovery in Astronomy
Authors: Kartheik G. Iyer, Mikaeel Yunus, Charles O'Neill, Christine Ye, Alina Hyk, Kiera McCormick, Ioana Ciucă, John F. Wu, Alberto Accomazzi, Simone Astarita, Rishabh Chakrabarty, Jesse Cranney, Anjalie Field, Tirthankar Ghosal, Michele Ginolfi, Marc Huertas-Company, Maja Jabłońska, Sandor Kruk, Huiling Liu, Gabriel Marchidan, Rohit Mistry, J. P. Naiman, J. E. G. Peek, Mugdha Polimera, Sergio J. Rodríguez Méndez, Kevin Schawinski, Sanjib Sharma, Michael J. Smith, Yuan-Sen Ting, Mike Walmsley
Figure caption: The impact of various facilities in their specific domains and beyond. Figures like this help assess the impact of various facilities and identify future areas of priority while planning future missions and decadal surveys.
Paper:  pathfinder: A Semantic Framework for Literature Review and Knowledge Discovery in Astronomy
Authors: Kartheik G. Iyer, Mikaeel Yunus, Charles O'Neill, Christine Ye, Alina Hyk, Kiera McCormick, Ioana Ciucă, John F. Wu, Alberto Accomazzi, Simone Astarita, Rishabh Chakrabarty, Jesse Cranney, Anjalie Field, Tirthankar Ghosal, Michele Ginolfi, Marc Huertas-Company, Maja Jabłońska, Sandor Kruk, Huiling Liu, Gabriel Marchidan, Rohit Mistry, J. P. Naiman, J. E. G. Peek, Mugdha Polimera, Sergio J. Rodríguez Méndez, Kevin Schawinski, Sanjib Sharma, Michael J. Smith, Yuan-Sen Ting, Mike Walmsley
Figure caption: Top-k retrieved papers for three different example queries, visualized in the two-dimensional UMAP space. Red points are outliers; blue points are nonoutliers. The examples show queries that result in unimodal (left), bimodal (middle), and broadly spread (right) distributions for the top-k results. Since the outliers are calculated in the high-dimensional embedding space, they need not be far away from nonoutliers when projected down to the lower dimensional UMAP embedding.
Paper:  pathfinder: A Semantic Framework for Literature Review and Knowledge Discovery in Astronomy
Authors: Kartheik G. Iyer, Mikaeel Yunus, Charles O'Neill, Christine Ye, Alina Hyk, Kiera McCormick, Ioana Ciucă, John F. Wu, Alberto Accomazzi, Simone Astarita, Rishabh Chakrabarty, Jesse Cranney, Anjalie Field, Tirthankar Ghosal, Michele Ginolfi, Marc Huertas-Company, Maja Jabłońska, Sandor Kruk, Huiling Liu, Gabriel Marchidan, Rohit Mistry, J. P. Naiman, J. E. G. Peek, Mugdha Polimera, Sergio J. Rodríguez Méndez, Kevin Schawinski, Sanjib Sharma, Michael J. Smith, Yuan-Sen Ting, Mike Walmsley
Figure caption: Schematic showing the overall pathfinder pipeline.
Paper: The AstroSat UV Deep Field South. I. Far- and Near-ultraviolet Source Catalog of the GOODS South Region
Authors: Kanak Saha, Soumil Maulick, Pushpak Pandey, Souradeep Bhattacharya, Anshuman Borgohain, Chayan Mondal, Marc Rafelski, Manish Kataria, Harry I. Teplitz, Shyam N. Tandon, Rogier A. Windhorst, Bruce G. Elmegreen, Edmund Christian Herenz, Michael Rutkowski
Figure caption: Left panel: N242W magnitude of sources detected in the negative image (with and without a filter) of the AUDFs field. Two sources detected in our final version are fainter than the 3σ  detection limit. Right panel: distribution of fluxes within 1000 randomly placed apertures having a PSF FWHM diameter, on empty regions, across the F154W (red) and N242W (blue) UVIT images. Note that the flux units are normalized to the sky background rms. npix denotes the number of pixels in the aperture.
Paper: The AstroSat UV Deep Field South. I. Far- and Near-ultraviolet Source Catalog of the GOODS South Region
Authors: Kanak Saha, Soumil Maulick, Pushpak Pandey, Souradeep Bhattacharya, Anshuman Borgohain, Chayan Mondal, Marc Rafelski, Manish Kataria, Harry I. Teplitz, Shyam N. Tandon, Rogier A. Windhorst, Bruce G. Elmegreen, Edmund Christian Herenz, Michael Rutkowski
Figure caption: Top two rows: a comparison of GALEX NUV and UVIT NUV observation with HST/F606W filter image as the optical reference. The third, fourth, and fifth rows: central UV emission from a local elliptical (E0) galaxy in the N242W filter. HST/F606W and JWST/F277W images are shown to confirm the morphology; the radius of the black circle is 4.″5. The red circle denotes another early-type galaxy at z = 0.27. Middle row: an interacting spiral galaxy at z ≃ 1 in N242W filter, circle size 2.″5. HST/F606W and JWST/F277W images are shown for the sake of comparison. Bottom row: UVIT FUV image of a barred spiral galaxy at z ≃ 0.21; blue circle size 3.″5
Paper: The AstroSat UV Deep Field South. I. Far- and Near-ultraviolet Source Catalog of the GOODS South Region
Authors: Kanak Saha, Soumil Maulick, Pushpak Pandey, Souradeep Bhattacharya, Anshuman Borgohain, Chayan Mondal, Marc Rafelski, Manish Kataria, Harry I. Teplitz, Shyam N. Tandon, Rogier A. Windhorst, Bruce G. Elmegreen, Edmund Christian Herenz, Michael Rutkowski
Figure caption: Source-count distribution (shown are mag > 26) of detected objects as a function of circular aperture magnitudes in the ﹩4\times 4\ {\mathrm{arcmin}}^{2}﹩ real UVIT (black histogram) field and in the mock Poisson background fields (colored histograms) for F154W (left panel) and N242W (right panel). All noise peaks detected objects resulting from background fluctuations in the Poisson-generated images are fainter than 26 mag in both bands. The gray dashed lines indicate the 3σ detection limits for the deep regions of the N242W and F154W bands. The bin size is 0.25 mag.
Paper: The AstroSat UV Deep Field South. I. Far- and Near-ultraviolet Source Catalog of the GOODS South Region
Authors: Kanak Saha, Soumil Maulick, Pushpak Pandey, Souradeep Bhattacharya, Anshuman Borgohain, Chayan Mondal, Marc Rafelski, Manish Kataria, Harry I. Teplitz, Shyam N. Tandon, Rogier A. Windhorst, Bruce G. Elmegreen, Edmund Christian Herenz, Michael Rutkowski
Figure caption: Source-count distribution (red: F154W, blue: N242W) of objects having a joint HLF and F154W flag = 1 in the N242W crossmatched catalog. The measured source magnitudes are not aperture corrected.
Paper: The AstroSat UV Deep Field South. I. Far- and Near-ultraviolet Source Catalog of the GOODS South Region
Authors: Kanak Saha, Soumil Maulick, Pushpak Pandey, Souradeep Bhattacharya, Anshuman Borgohain, Chayan Mondal, Marc Rafelski, Manish Kataria, Harry I. Teplitz, Shyam N. Tandon, Rogier A. Windhorst, Bruce G. Elmegreen, Edmund Christian Herenz, Michael Rutkowski
Figure caption: Examples of candidate LyC leakers caught in F154W (upper and middle panels) and N242W (bottom panel) filters from the AUDFs field. The radius of the dark circle in each panel is 1.″6. The green square indicates the on-sky position of these galaxies taken from the HST/G141 grism survey (I. G. Momcheva et al. 2016).
Paper: Mass-loss Rate of Highly Evolved Stars in the Magellanic Clouds
Authors: Jing Wen, 静 文, Ming Yang, 明 杨, Jian Gao, 健 高, Bingqiu Chen, 丙秋 陈, Yi Ren, 逸 任, Biwei Jiang, 碧沩 姜
Figure caption: Two examples of modifying classification after visual inspection are shown. Observational data are denoted using various symbols and colors, while the best-fit model is represented as a solid black curve. The contributions from the central star and circumstellar dust are depicted by the black dashed and dotted–dashed lines, respectively. Additionally, the blue dashed line represents the model with the minimum χ 2 for another chemical type. In the left panel, the original best-fit model is C-rich (blue dashed line), which may be due to the continuous rise in the infrared band. After crossmatching with the IRS, we found that this RSG has weak but prominent silicate emission peaks at both 9.7 and 18 μm, so we changed the best-fit model (black solid line). The right panel shows a source that we moved from S1 to S2. This source has obvious infrared emission, but lacks long-wavelength data, making it difficult to determine its type. Although its original best-fit model was C-rich (blue dashed line), after visual inspection we found a rising trend in the [8.0] band, which resembles the shape of an O-rich SED more closely. Therefore, we adjusted its classification.
Paper: Mass-loss Rate of Highly Evolved Stars in the Magellanic Clouds
Authors: Jing Wen, 静 文, Ming Yang, 明 杨, Jian Gao, 健 高, Bingqiu Chen, 丙秋 陈, Yi Ren, 逸 任, Biwei Jiang, 碧沩 姜
Figure caption: Examples of SED fitting for eight AGBs in the LMC. The first, second, and third rows show good SED fitting for Op-thin, C-rich, and O-rich stars, respectively (sflag = 0). The bottom row shows anomalous SEDs of two sources. The left panel shows a source that was removed during the data filtering process (sflag = 1), while the right panel shows a source with possible variability (sflag = 0).
Paper: Mass-loss Rate of Highly Evolved Stars in the Magellanic Clouds
Authors: Jing Wen, 静 文, Ming Yang, 明 杨, Jian Gao, 健 高, Bingqiu Chen, 丙秋 陈, Yi Ren, 逸 任, Biwei Jiang, 碧沩 姜
Figure caption: Examples of SED fitting for eight RSGs in the SMC. Rows 1 to 3 show good fitting for Op-thin, C-rich, and O-rich stars (sflag = 0), while the bottom row shows anomalous fitting due to bad W3/W4 data (left, sflag = 3) and possible binary or other factors (right, sflag = 2).
Paper: Mass-loss Rate of Highly Evolved Stars in the Magellanic Clouds
Authors: Jing Wen, 静 文, Ming Yang, 明 杨, Jian Gao, 健 高, Bingqiu Chen, 丙秋 陈, Yi Ren, 逸 任, Biwei Jiang, 碧沩 姜
Figure caption: Histogram of numbers of data points for the sample.
Paper: Mass-loss Rate of Highly Evolved Stars in the Magellanic Clouds
Authors: Jing Wen, 静 文, Ming Yang, 明 杨, Jian Gao, 健 高, Bingqiu Chen, 丙秋 陈, Yi Ren, 逸 任, Biwei Jiang, 碧沩 姜
Figure caption: Luminosity–MLR diagrams for different types of evolved stars in MCs, where light gray represents sources in the LMC and dark gray represents sources in the SMC. The red lines represent our fitted prescription. The lines with various colors represent the prescriptions derived from previous studies (D. Reimers 1975; A. Wachter et al. 2002; J. T. van Loon et al. 2005).
Paper: Mass-loss Rate of Highly Evolved Stars in the Magellanic Clouds
Authors: Jing Wen, 静 文, Ming Yang, 明 杨, Jian Gao, 健 高, Bingqiu Chen, 丙秋 陈, Yi Ren, 逸 任, Biwei Jiang, 碧沩 姜
Figure caption: Diagrams depicting the relations between DPR and pulsation parameters for AGBs (sflag = 0) in the LMC (left) and SMC (right). The first row illustrates the changes in AGB types with the evolution of pulsation sequences. The second row shows the change in DPR on the period–[3.6] diagram. The third row shows the variation of DPR on the period–amplitude diagram.
Paper: Mass-loss Rate of Highly Evolved Stars in the Magellanic Clouds
Authors: Jing Wen, 静 文, Ming Yang, 明 杨, Jian Gao, 健 高, Bingqiu Chen, 丙秋 陈, Yi Ren, 逸 任, Biwei Jiang, 碧沩 姜
Figure caption: ([3.6] – [8.0])0 and (J – [3.6])0 color versus MLR diagrams for the RSGs (gray dots), O-rich AGBs (blue dots), C-rich AGBs (red dots), and x-AGBs (green dots). Only sources with sflag = 0 and not Op-thin are included. The color–DPR relation obtained from previous work is represented by black lines (M. Matsuura et al. 2009; D. Riebel et al. 2012; M. A. T. Groenewegen & G. C. Sloan 2018).
Paper: Mass-loss Rate of Highly Evolved Stars in the Magellanic Clouds
Authors: Jing Wen, 静 文, Ming Yang, 明 杨, Jian Gao, 健 高, Bingqiu Chen, 丙秋 陈, Yi Ren, 逸 任, Biwei Jiang, 碧沩 姜
Figure caption: Projected pulsation period vs. amplitude diagram. The period is replaced with the parameter ﹩{\rm{log}}(P[{W}_{{JK}}=12])﹩.
Paper: Mass-loss Rate of Highly Evolved Stars in the Magellanic Clouds
Authors: Jing Wen, 静 文, Ming Yang, 明 杨, Jian Gao, 健 高, Bingqiu Chen, 丙秋 陈, Yi Ren, 逸 任, Biwei Jiang, 碧沩 姜
Figure caption: Luminosity–MLR diagrams for different types of AGBs in the LMC. The top panels show the luminosity derived from integrating the best-fit model SED (﹩{L}_{\mathrm{mod}}﹩), while the bottom panels show the luminosity derived from integrating the observed SED (L obs).
Paper: Mass-loss Rate of Highly Evolved Stars in the Magellanic Clouds
Authors: Jing Wen, 静 文, Ming Yang, 明 杨, Jian Gao, 健 高, Bingqiu Chen, 丙秋 陈, Yi Ren, 逸 任, Biwei Jiang, 碧沩 姜
Figure caption: Same as Figure 15 but for AGBs in the SMC.
Paper: ALMA Lensing Cluster Survey: Deep 1.2 mm Number Counts and Infrared Luminosity Functions at z ≃ 1–8
Authors: Seiji Fujimoto, Kotaro Kohno, Masami Ouchi, Masamune Oguri, Vasily Kokorev, Gabriel Brammer, Fengwu Sun, Jorge González-López, Franz E. Bauer, Gabriel B. Caminha, Bunyo Hatsukade, Johan Richard, Ian Smail, Akiyoshi Tsujita, Yoshihiro Ueda, Ryosuke Uematsu, Adi Zitrin, Dan Coe, Jean-Paul Kneib, Marc Postman, Keiichi Umetsu, Claudia del P. Lagos, Gergö Popping, Yiping Ao, Larry Bradley, Karina Caputi, Miroslava Dessauges-Zavadsky, Eiichi Egami, Daniel Espada, R. J. Ivison, Mathilde Jauzac, Kirsten K. Knudsen, Anton M. Koekemoer, Georgios E. Magdis, Guillaume Mahler, A. M. Muñoz Arancibia, Timothy Rawle, Kazuhiro Shimasaku, Sune Toft, Hideki Umehata, Francesco Valentino, Tao Wang, Wei-Hao Wang
Figure caption: Differential number counts at 1.2 mm. The red open circles and pentagons are the number counts derived from our ALCS blind and blind+prior samples without the MC simulations, respectively, where the error bars only take Poisson uncertainties into account. The filled red circles represent the number counts corrected by the MC simulations that implement all relevant uncertainties, such as redshift, magnification, and flux density measurements, where the error bars indicate the 16–84th percentile in the 1000 MC realizations. The solid red line and the shaded region denote our fiducial Schechter function estimate and the associated 1σ error, while the dashed magenta line presents our fiducial DPL function estimate. In the fitting, we use our number-count estimates alone to avoid potential systematic uncertainty in different measurements from different surveys. For comparison, we also show previous ALMA submillimeter/millimeter number counts in the literature (Karim et al. 2013; Hatsukade et al. 2014; Ono et al. 2014; Carniani et al. 2015; Fujimoto et al. 2016; Umehata et al. 2017; Franco et al. 2018; Hatsukade et al. 2018; Muñoz Arancibia et al. 2018; Stach et al. 2018; Béthermin et al. 2020; González-López et al. 2020; Gómez-Guijarro et al. 2022; Muñoz Arancibia et al. 2023). The black dashed line is the best-fit Schechter function using the results obtained in GOODS-S (Gómez-Guijarro et al. 2022) and HUDF (ASPECS; González-López et al. 2020). The black solid line is taken from González-López et al. (2020) obtained from the P(D) analysis that indicates the presence of the flattening below ∼0.1 mJy; the black shaded region denotes the associated 1σ error. When comparing previous measurements of the number counts at different wavelengths to our 1.2 mm band, we scale the flux densities using the methods described in Section 5.2.
Paper: ALMA Lensing Cluster Survey: Deep 1.2 mm Number Counts and Infrared Luminosity Functions at z ≃ 1–8
Authors: Seiji Fujimoto, Kotaro Kohno, Masami Ouchi, Masamune Oguri, Vasily Kokorev, Gabriel Brammer, Fengwu Sun, Jorge González-López, Franz E. Bauer, Gabriel B. Caminha, Bunyo Hatsukade, Johan Richard, Ian Smail, Akiyoshi Tsujita, Yoshihiro Ueda, Ryosuke Uematsu, Adi Zitrin, Dan Coe, Jean-Paul Kneib, Marc Postman, Keiichi Umetsu, Claudia del P. Lagos, Gergö Popping, Yiping Ao, Larry Bradley, Karina Caputi, Miroslava Dessauges-Zavadsky, Eiichi Egami, Daniel Espada, R. J. Ivison, Mathilde Jauzac, Kirsten K. Knudsen, Anton M. Koekemoer, Georgios E. Magdis, Guillaume Mahler, A. M. Muñoz Arancibia, Timothy Rawle, Kazuhiro Shimasaku, Sune Toft, Hideki Umehata, Francesco Valentino, Tao Wang, Wei-Hao Wang
Figure caption: Intrinsic ALMA flux density (S int) and redshift distributions of the ALCS sources after the lens correction. The red-filled circles indicate the 146 ALCS sources after removing the cluster member galaxies and adopting the average intrinsic flux density for multiply imaged systems. The spectroscopically confirmed sources are marked with red open circles. The color crosses denote ALMA sources identified in other recent ALMA surveys—707 sources from Band 7 (870 μm) snapshot follow-up observations for SCUBA2 sources in UDS (AS2UDS; Dudzevičiūtė et al. 2020), 34 sources from Band 6 deep blind observations in HUDF (ASPECS; González-López et al. 2020), 88 sources from Band 6 wide blind observations in GOODS-S (A2GS; Gómez-Guijarro et al. 2022), and 12 sources from Band 4 (2 mm) wide blind observations in COSMOS (MORA; Casey et al. 2021). For the AS2UDS and MORA sources, we scale their flux density by assuming a modified blackbody based on their best-fit T d and β  d  values presented in the literature. The top and right panels present the probability distribution for the redshift and intrinsic flux density, where the peaks are normalized. The solid lines are the median value for each sample. The dashed and dotted lines show the median values for the spectroscopic and photometric samples in the ALCS sources, respectively, which show good agreement with each other and indicate that their potential difference is negligible owing to the lensing support.
Paper: ALMA Lensing Cluster Survey: Deep 1.2 mm Number Counts and Infrared Luminosity Functions at z ≃ 1–8
Authors: Seiji Fujimoto, Kotaro Kohno, Masami Ouchi, Masamune Oguri, Vasily Kokorev, Gabriel Brammer, Fengwu Sun, Jorge González-López, Franz E. Bauer, Gabriel B. Caminha, Bunyo Hatsukade, Johan Richard, Ian Smail, Akiyoshi Tsujita, Yoshihiro Ueda, Ryosuke Uematsu, Adi Zitrin, Dan Coe, Jean-Paul Kneib, Marc Postman, Keiichi Umetsu, Claudia del P. Lagos, Gergö Popping, Yiping Ao, Larry Bradley, Karina Caputi, Miroslava Dessauges-Zavadsky, Eiichi Egami, Daniel Espada, R. J. Ivison, Mathilde Jauzac, Kirsten K. Knudsen, Anton M. Koekemoer, Georgios E. Magdis, Guillaume Mahler, A. M. Muñoz Arancibia, Timothy Rawle, Kazuhiro Shimasaku, Sune Toft, Hideki Umehata, Francesco Valentino, Tao Wang, Wei-Hao Wang
Figure caption: Example of the line emitters serendipitously detected among the ALCS continuum sources. We evaluate the EW and subtract the line contributions to the continuum flux measurement in our analysis (Section 3.4). Left: ALCS 15 GHz wide spectrum in ALMA Band 6. Lines are clearly detected at ∼269 GHz among three-line emitters identified in the M0553 cluster. Right: HST color image for M0553-C133/190/249, using F814W (blue), F125W (green), and F160W (red) filters. Red contours show the line intensity drawn at 6σ, 8σ, and 10σ. The counterparts of the line emitters are a triplet multiple-imaged system spectroscopically confirmed at z = 1.14 (Ebeling et al. 2017), concluding that the millimeter line is CO(5–4).