adsabs/AstroCLIMB huggingface dataset:
Paper: Spatially Offset Active Galactic Nuclei in the Very Large Array Sky Survey: Tracers of Galaxy Mergers and Wandering Massive Black Holes
Authors: R. Scott Barrows, Julia M. Comerford
Figure caption: Offset AGN occupation fraction (fOA = NOA/NGal) against host galaxy stellar mass (M⋆,Host). Vertical error bars denote the binomial uncertainties, and horizontal error bars denote the bin widths. Subsamples are shown for redshift limits of z < 0.1, 0.2, and 0.3 that are complete in M⋆,Host (Figure 4). For comparison, also shown are the ROMULUS simulation predictions from A. Ricarte et al. (2021a; R21, for z = 0.5; green, dotted) for offset MBHs, assuming the halo-to-stellar mass ratio of the Milky Way (T. C. Licquia & J. A. Newman 2015; L. Posti & A. Helmi 2019), the galaxy pair fractions from A. S. G. Robotham et al. (2014; R14; purple, solid), and K. R. V. Casteels et al. (2014; C14; blue, dashed), each rebinned to the abscissa grid for our sample. All samples are normalized to a sum of unity over the range M⋆,Host = 1010–1012 M⊙. The dashed vertical (gray) line denotes the Milky Way stellar mass. Compared to predictions, the sample from this work implies a larger fraction of offset MBHs will be in lower-mass galaxies.
Paper: Spatially Offset Active Galactic Nuclei in the Very Large Array Sky Survey: Tracers of Galaxy Mergers and Wandering Massive Black Holes
Authors: R. Scott Barrows, Julia M. Comerford
Figure caption: Offset AGN occupation fraction (fOA = NOA/NGal) against angular offset, normalized by the host galaxy Petrosian radius (ΔΘ/rpetro), out to 2 (upper selection limit; Section 2.2). Vertical error bars denote the binomial uncertainties, and horizontal errorbars denote the bin widths. Subsamples are shown for redshift limits of z < 0.1, 0.2, and 0.3 that are complete in ΔS (Figure 4). For comparison, also shown are the predictions from ROMULUS25 (M. Tremmel et al. 2018a; T18; green, dotted) and IllustrisTNG (E. J. Weller et al. 2022; W22; blue, solid), each rebinned to the abscissa grid for our sample and assuming the half-light radius of the Milky Way (J. Lian et al. 2024) and the conversion to Petrosian radius (M. A. Strauss et al. 2002). All samples are normalized to a sum of unity over the range ΔΘ / rpetro = 0.3–2. The dashed vertical (gray) line denotes 10% of the Milky Way Virial radius (W. Dehnen et al. 2006). At all relative offsets, the sample from this work is consistent with both simulations within 2σ for all redshift limits.
Paper: Spatially Offset Active Galactic Nuclei in the Very Large Array Sky Survey: Tracers of Galaxy Mergers and Wandering Massive Black Holes
Authors: R. Scott Barrows, Julia M. Comerford
Figure caption: Cumulative offset MBH occupation fraction (NMBH/NGal) against MBH mass (M•) for our sample (subset at z < 0.1 that is complete for ΔS > 5 kpc). M• estimates are based on Eddington ratios of fEdd = 0.1, 0.5, and 1, and values of NMBH/NGal are obtained by normalizing the offset AGN fractions (corrected for background/foreground source contamination) by the VLASS AGN fraction among our sample (see Section 8 for details). For comparison, also shown are predictions from the L-Galaxies simulation (J. Untzaga et al. 2024; U24) for pairing, disrupted, and recoil/slingshot offset MBHs (green, purple, and magenta hexagons, respectively), and the SatGen (F. Jiang et al. 2021) predictions from J. E. Greene et al. (2021; G21) assuming all accreted satellites host a MBH with M• based on the MBH–Mσ relation (gray, solid). We also show upper limits for the Milky Way (G21). The observed values of NMBH/NGal are systematically lower than the predictions based on satellites but potentially consistent with observed upper limits for the Milky Way.
Paper: Spatially Offset Active Galactic Nuclei in the Very Large Array Sky Survey: Tracers of Galaxy Mergers and Wandering Massive Black Holes
Authors: R. Scott Barrows, Julia M. Comerford
Figure caption: Excess of the fraction of offset AGN candidates in galaxy groups relative to that of the parent AGN (Δgrp = fgrp,OA / fgrp,A) against richness of their environments (i.e., number of group member galaxies; Nrich). Vertical errorbars denote binomial uncertainties and horizontal errorbars denote the bin widths. The group membership classifications are obtained by matching the host galaxies to the catalogs from A. A. Berlind et al. (2006; B06; green diamonds), E. Tempel et al. (2012; T12; purple squares), and Z. L. Wen et al. (2012; W12; blue circles). The horizontal dashed line indicates Δgrp = 1. In each Nrich bin, the values of Δgrp are consistent between each sample to within the uncertainties. An excess in Δgrp is observed at Nrich > 100 (common galaxy cluster lower threshold), which may suggest a potential selection toward dense environments. The middle and bottom panels show the distributions of the parent and offset AGN samples, respectively (each normalized to a sum of unity), where the vast majority are not in clusters.
Paper: Spatially Offset Active Galactic Nuclei in the Very Large Array Sky Survey: Tracers of Galaxy Mergers and Wandering Massive Black Holes
Authors: R. Scott Barrows, Julia M. Comerford
Figure caption: Radio spectral indices (α) against (from left to right) host galaxy redshift (z), host galaxy star formation rate (SFR), host galaxy stellar mass (M⋆,Host), and observed AGN 2−4 GHz luminosity (L2−4) for the offset AGN candidates with α measurements (those in the CIRADA single epoch catalog for Epoch 2). The value of α = −0.8, commonly used for separating radio jets (α < −0.8) from radio cores (α > −0.8), is shown as a black dashed line, and the median uncertainty of the α values is denoted in the left panel. The offset AGN candidates are shown as magenta circles (α > −0.8) and orange squares (α < −0.8), and VLASS sources flagged as having extended morphologies (candidate radio jets) are denoted by the log-scale density plot. The candidate radio jets show a relative bias toward lower α values, 59% of which are <−0.8, compared to 47% for the offset AGN candidates.
Paper: Spatially Offset Active Galactic Nuclei in the Very Large Array Sky Survey: Tracers of Galaxy Mergers and Wandering Massive Black Holes
Authors: R. Scott Barrows, Julia M. Comerford
Figure caption: Offset AGN background/foreground contamination fraction (fcont) against host galaxy Petrosian radius (rpetro). Vertical errorbars denote binomial uncertainties, and horizontal errorbars denote the bin widths. Subsamples binned by redshift (z) are shown (horizontally offset for clarity), and the distributions are shown in the top panel with corresponding colors. Potential evidence for a positive dependence of fcont on rpetro is seen (Spearman rank correlation probability of 96% for the overall sample). When accounting for the uncertainties, fcont is consistent at all redshifts (for rpetro < 8″).
Paper: Parallel Application of Slitless Spectroscopy to Analyze Galaxy Evolution (PASSAGE): Survey Overview
Authors: Matthew A. Malkan, Vihang Mehta, Ayan Acharyya, Hollis B. Akins, Anahita Alavi, Hakim Atek, Ivano Baronchelli, Andrew J. Battisti, Kit Boyett, Marusa Bradac, Sean Tyler Bruton, Andrew J. Bunker, Adam J. Burgasser, Caitlin M. Casey, Nuo Chen, James Colbert, Y. Sophia Dai, Maximilien Franco, Clea Hannahs, Santosh Harish, Farhanul Hasan, Matthew J. Hayes, Alaina L. Henry, Mason Huberty, Tucker Jones, Jeyhan S. Kartaltepe, Keunho J. Kim, Nicha Leethochawalit, Jacob Levine, Sijia Li, Yu-Heng Lin, Yixiao Liu, Charlotte Mason, Daniel Masters, Henry Joy McCracken, Takahiro Morishita, Kalina V. Nedkova, Marc Rafelski, Vivasvaan Aditya Raj, Guido Roberts-Borsani, Axel Runnholm, Michael J. Rutkowski, Alberto Saldana-Lopez, Zahra Sattari, Claudia Scarlata, Kasper Borello Schmidt, Marko Shuntov, Harry Teplitz, Michele Trenti, Tommaso Treu, Benedetta Vulcani, Peter J. Watson, Xin Wang, Zhuyun Zhuang
Figure caption: Sky locations of the final observed 63 PASSAGE fields, shown in Equatorial coordinates. Note that some fields overlap on the scale of this diagram. In particular, the 18 PASSAGE fields in the COSMOS field all overlap in a single yellow box in this low-resolution sky map. These are resolved in the zoom-in of the COSMOS region shown in Figure 2.
Paper: Parallel Application of Slitless Spectroscopy to Analyze Galaxy Evolution (PASSAGE): Survey Overview
Authors: Matthew A. Malkan, Vihang Mehta, Ayan Acharyya, Hollis B. Akins, Anahita Alavi, Hakim Atek, Ivano Baronchelli, Andrew J. Battisti, Kit Boyett, Marusa Bradac, Sean Tyler Bruton, Andrew J. Bunker, Adam J. Burgasser, Caitlin M. Casey, Nuo Chen, James Colbert, Y. Sophia Dai, Maximilien Franco, Clea Hannahs, Santosh Harish, Farhanul Hasan, Matthew J. Hayes, Alaina L. Henry, Mason Huberty, Tucker Jones, Jeyhan S. Kartaltepe, Keunho J. Kim, Nicha Leethochawalit, Jacob Levine, Sijia Li, Yu-Heng Lin, Yixiao Liu, Charlotte Mason, Daniel Masters, Henry Joy McCracken, Takahiro Morishita, Kalina V. Nedkova, Marc Rafelski, Vivasvaan Aditya Raj, Guido Roberts-Borsani, Axel Runnholm, Michael J. Rutkowski, Alberto Saldana-Lopez, Zahra Sattari, Claudia Scarlata, Kasper Borello Schmidt, Marko Shuntov, Harry Teplitz, Michele Trenti, Tommaso Treu, Benedetta Vulcani, Peter J. Watson, Xin Wang, Zhuyun Zhuang
Figure caption: Example of an extreme emission-line galaxy from the Par 1 field. The upper left panel shows the broadband direct image, 1﹩\mathop{.}\limits^{\unicode{x02033}}﹩28 on a side (32 × 32 pixels at 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩04 pixel−1), drizzled with grizli and oriented with north up. The lower rectangular panel shows the two-dimensional spectrogram at the native 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩066 pixel−1 scale, and the upper right displays the extracted one-dimensional spectrum. The flux scale is unreliable near the blue/red ends of each filter, shown by the full vertical gray rectangles.
Paper: Parallel Application of Slitless Spectroscopy to Analyze Galaxy Evolution (PASSAGE): Survey Overview
Authors: Matthew A. Malkan, Vihang Mehta, Ayan Acharyya, Hollis B. Akins, Anahita Alavi, Hakim Atek, Ivano Baronchelli, Andrew J. Battisti, Kit Boyett, Marusa Bradac, Sean Tyler Bruton, Andrew J. Bunker, Adam J. Burgasser, Caitlin M. Casey, Nuo Chen, James Colbert, Y. Sophia Dai, Maximilien Franco, Clea Hannahs, Santosh Harish, Farhanul Hasan, Matthew J. Hayes, Alaina L. Henry, Mason Huberty, Tucker Jones, Jeyhan S. Kartaltepe, Keunho J. Kim, Nicha Leethochawalit, Jacob Levine, Sijia Li, Yu-Heng Lin, Yixiao Liu, Charlotte Mason, Daniel Masters, Henry Joy McCracken, Takahiro Morishita, Kalina V. Nedkova, Marc Rafelski, Vivasvaan Aditya Raj, Guido Roberts-Borsani, Axel Runnholm, Michael J. Rutkowski, Alberto Saldana-Lopez, Zahra Sattari, Claudia Scarlata, Kasper Borello Schmidt, Marko Shuntov, Harry Teplitz, Michele Trenti, Tommaso Treu, Benedetta Vulcani, Peter J. Watson, Xin Wang, Zhuyun Zhuang
Figure caption: Pie chart showing the distribution of overlap percentages across different JWST filters (F115W, F150W, F200W) used in PASSAGE. The inner ring divides the observations into spectra with one, two, and three filters. The outer rings further separate these observations into those observed with a single grism (“1 PA,” signifying that the spectra are dispersed at a single position angle) and those observed with both the GR150R and GR150C grisms. The total numbers of fields in each category are given in parentheses. The total numbers in the wheel sum up to 67, rather than 63, due to the four fields, such as Par027, that were observed with two different combinations of filters and orientations.
Paper: Parallel Application of Slitless Spectroscopy to Analyze Galaxy Evolution (PASSAGE): Survey Overview
Authors: Matthew A. Malkan, Vihang Mehta, Ayan Acharyya, Hollis B. Akins, Anahita Alavi, Hakim Atek, Ivano Baronchelli, Andrew J. Battisti, Kit Boyett, Marusa Bradac, Sean Tyler Bruton, Andrew J. Bunker, Adam J. Burgasser, Caitlin M. Casey, Nuo Chen, James Colbert, Y. Sophia Dai, Maximilien Franco, Clea Hannahs, Santosh Harish, Farhanul Hasan, Matthew J. Hayes, Alaina L. Henry, Mason Huberty, Tucker Jones, Jeyhan S. Kartaltepe, Keunho J. Kim, Nicha Leethochawalit, Jacob Levine, Sijia Li, Yu-Heng Lin, Yixiao Liu, Charlotte Mason, Daniel Masters, Henry Joy McCracken, Takahiro Morishita, Kalina V. Nedkova, Marc Rafelski, Vivasvaan Aditya Raj, Guido Roberts-Borsani, Axel Runnholm, Michael J. Rutkowski, Alberto Saldana-Lopez, Zahra Sattari, Claudia Scarlata, Kasper Borello Schmidt, Marko Shuntov, Harry Teplitz, Michele Trenti, Tommaso Treu, Benedetta Vulcani, Peter J. Watson, Xin Wang, Zhuyun Zhuang
Figure caption: Zoom-in on PASSAGE fields located in and around the COSMOS field. The background is the Hubble ACS mosaic of the COSMOS field (A. M. Koekemoer et al. 2007; N. Scoville et al. 2007), along with the deep CANDELS survey as a red outline (N. A. Grogin et al. 2011; A. M. Koekemoer et al. 2011). The orange outline shows the UltraVISTA imaging survey footprint of the COSMOS field (H. J. McCracken et al. 2012). The blue and green outlines are the COSMOS-Web NIRCam and MIRI coverage, respectively (C. M. Casey et al. 2023). The magenta outline is the coverage of the PRIMER JWST survey (GO #1837).
Paper: Parallel Application of Slitless Spectroscopy to Analyze Galaxy Evolution (PASSAGE): Survey Overview
Authors: Matthew A. Malkan, Vihang Mehta, Ayan Acharyya, Hollis B. Akins, Anahita Alavi, Hakim Atek, Ivano Baronchelli, Andrew J. Battisti, Kit Boyett, Marusa Bradac, Sean Tyler Bruton, Andrew J. Bunker, Adam J. Burgasser, Caitlin M. Casey, Nuo Chen, James Colbert, Y. Sophia Dai, Maximilien Franco, Clea Hannahs, Santosh Harish, Farhanul Hasan, Matthew J. Hayes, Alaina L. Henry, Mason Huberty, Tucker Jones, Jeyhan S. Kartaltepe, Keunho J. Kim, Nicha Leethochawalit, Jacob Levine, Sijia Li, Yu-Heng Lin, Yixiao Liu, Charlotte Mason, Daniel Masters, Henry Joy McCracken, Takahiro Morishita, Kalina V. Nedkova, Marc Rafelski, Vivasvaan Aditya Raj, Guido Roberts-Borsani, Axel Runnholm, Michael J. Rutkowski, Alberto Saldana-Lopez, Zahra Sattari, Claudia Scarlata, Kasper Borello Schmidt, Marko Shuntov, Harry Teplitz, Michele Trenti, Tommaso Treu, Benedetta Vulcani, Peter J. Watson, Xin Wang, Zhuyun Zhuang
Figure caption: Emission-line flux sensitivity in typical PASSAGE observations. The 5σ detection limits, in erg s–1 cm−2 are shown for point sources in several representative fields, with integration times ranging from our shortest to our longest exposures.
Paper: Parallel Application of Slitless Spectroscopy to Analyze Galaxy Evolution (PASSAGE): Survey Overview
Authors: Matthew A. Malkan, Vihang Mehta, Ayan Acharyya, Hollis B. Akins, Anahita Alavi, Hakim Atek, Ivano Baronchelli, Andrew J. Battisti, Kit Boyett, Marusa Bradac, Sean Tyler Bruton, Andrew J. Bunker, Adam J. Burgasser, Caitlin M. Casey, Nuo Chen, James Colbert, Y. Sophia Dai, Maximilien Franco, Clea Hannahs, Santosh Harish, Farhanul Hasan, Matthew J. Hayes, Alaina L. Henry, Mason Huberty, Tucker Jones, Jeyhan S. Kartaltepe, Keunho J. Kim, Nicha Leethochawalit, Jacob Levine, Sijia Li, Yu-Heng Lin, Yixiao Liu, Charlotte Mason, Daniel Masters, Henry Joy McCracken, Takahiro Morishita, Kalina V. Nedkova, Marc Rafelski, Vivasvaan Aditya Raj, Guido Roberts-Borsani, Axel Runnholm, Michael J. Rutkowski, Alberto Saldana-Lopez, Zahra Sattari, Claudia Scarlata, Kasper Borello Schmidt, Marko Shuntov, Harry Teplitz, Michele Trenti, Tommaso Treu, Benedetta Vulcani, Peter J. Watson, Xin Wang, Zhuyun Zhuang
Figure caption: A high-redshift (z ≈ 4.6) compact galaxy from Par 28, shown in the same format as Figure 5. Strong broad rest-frame UV features including C III] λ1909 and Mg II λ2800 indicate this is a quasar.
Paper: Parallel Application of Slitless Spectroscopy to Analyze Galaxy Evolution (PASSAGE): Survey Overview
Authors: Matthew A. Malkan, Vihang Mehta, Ayan Acharyya, Hollis B. Akins, Anahita Alavi, Hakim Atek, Ivano Baronchelli, Andrew J. Battisti, Kit Boyett, Marusa Bradac, Sean Tyler Bruton, Andrew J. Bunker, Adam J. Burgasser, Caitlin M. Casey, Nuo Chen, James Colbert, Y. Sophia Dai, Maximilien Franco, Clea Hannahs, Santosh Harish, Farhanul Hasan, Matthew J. Hayes, Alaina L. Henry, Mason Huberty, Tucker Jones, Jeyhan S. Kartaltepe, Keunho J. Kim, Nicha Leethochawalit, Jacob Levine, Sijia Li, Yu-Heng Lin, Yixiao Liu, Charlotte Mason, Daniel Masters, Henry Joy McCracken, Takahiro Morishita, Kalina V. Nedkova, Marc Rafelski, Vivasvaan Aditya Raj, Guido Roberts-Borsani, Axel Runnholm, Michael J. Rutkowski, Alberto Saldana-Lopez, Zahra Sattari, Claudia Scarlata, Kasper Borello Schmidt, Marko Shuntov, Harry Teplitz, Michele Trenti, Tommaso Treu, Benedetta Vulcani, Peter J. Watson, Xin Wang, Zhuyun Zhuang
Figure caption: A line-rich EELG from the Par 28 field, shown in the same format as Figure 5. The object exhibits strong [O III], [O II], and Balmer emission from Hγ through Hα, visible across all three grism filters.
Paper: Parallel Application of Slitless Spectroscopy to Analyze Galaxy Evolution (PASSAGE): Survey Overview
Authors: Matthew A. Malkan, Vihang Mehta, Ayan Acharyya, Hollis B. Akins, Anahita Alavi, Hakim Atek, Ivano Baronchelli, Andrew J. Battisti, Kit Boyett, Marusa Bradac, Sean Tyler Bruton, Andrew J. Bunker, Adam J. Burgasser, Caitlin M. Casey, Nuo Chen, James Colbert, Y. Sophia Dai, Maximilien Franco, Clea Hannahs, Santosh Harish, Farhanul Hasan, Matthew J. Hayes, Alaina L. Henry, Mason Huberty, Tucker Jones, Jeyhan S. Kartaltepe, Keunho J. Kim, Nicha Leethochawalit, Jacob Levine, Sijia Li, Yu-Heng Lin, Yixiao Liu, Charlotte Mason, Daniel Masters, Henry Joy McCracken, Takahiro Morishita, Kalina V. Nedkova, Marc Rafelski, Vivasvaan Aditya Raj, Guido Roberts-Borsani, Axel Runnholm, Michael J. Rutkowski, Alberto Saldana-Lopez, Zahra Sattari, Claudia Scarlata, Kasper Borello Schmidt, Marko Shuntov, Harry Teplitz, Michele Trenti, Tommaso Treu, Benedetta Vulcani, Peter J. Watson, Xin Wang, Zhuyun Zhuang
Figure caption: A compact galaxy at z ≈ 3 from Par 28, shown in the same format as Figure 5. It displays moderate emission from [O II], [O III], and Hβ, offering useful spectral diagnostics at intermediate redshift.
Paper: Parallel Application of Slitless Spectroscopy to Analyze Galaxy Evolution (PASSAGE): Survey Overview
Authors: Matthew A. Malkan, Vihang Mehta, Ayan Acharyya, Hollis B. Akins, Anahita Alavi, Hakim Atek, Ivano Baronchelli, Andrew J. Battisti, Kit Boyett, Marusa Bradac, Sean Tyler Bruton, Andrew J. Bunker, Adam J. Burgasser, Caitlin M. Casey, Nuo Chen, James Colbert, Y. Sophia Dai, Maximilien Franco, Clea Hannahs, Santosh Harish, Farhanul Hasan, Matthew J. Hayes, Alaina L. Henry, Mason Huberty, Tucker Jones, Jeyhan S. Kartaltepe, Keunho J. Kim, Nicha Leethochawalit, Jacob Levine, Sijia Li, Yu-Heng Lin, Yixiao Liu, Charlotte Mason, Daniel Masters, Henry Joy McCracken, Takahiro Morishita, Kalina V. Nedkova, Marc Rafelski, Vivasvaan Aditya Raj, Guido Roberts-Borsani, Axel Runnholm, Michael J. Rutkowski, Alberto Saldana-Lopez, Zahra Sattari, Claudia Scarlata, Kasper Borello Schmidt, Marko Shuntov, Harry Teplitz, Michele Trenti, Tommaso Treu, Benedetta Vulcani, Peter J. Watson, Xin Wang, Zhuyun Zhuang
Figure caption: Another example of an extreme emission-line galaxy, displayed in the same layout as Figure 5. This compact galaxy from the Par 5 field shows a prominent Balmer series with emission visible up to Hϵ.
Paper: Parallel Application of Slitless Spectroscopy to Analyze Galaxy Evolution (PASSAGE): Survey Overview
Authors: Matthew A. Malkan, Vihang Mehta, Ayan Acharyya, Hollis B. Akins, Anahita Alavi, Hakim Atek, Ivano Baronchelli, Andrew J. Battisti, Kit Boyett, Marusa Bradac, Sean Tyler Bruton, Andrew J. Bunker, Adam J. Burgasser, Caitlin M. Casey, Nuo Chen, James Colbert, Y. Sophia Dai, Maximilien Franco, Clea Hannahs, Santosh Harish, Farhanul Hasan, Matthew J. Hayes, Alaina L. Henry, Mason Huberty, Tucker Jones, Jeyhan S. Kartaltepe, Keunho J. Kim, Nicha Leethochawalit, Jacob Levine, Sijia Li, Yu-Heng Lin, Yixiao Liu, Charlotte Mason, Daniel Masters, Henry Joy McCracken, Takahiro Morishita, Kalina V. Nedkova, Marc Rafelski, Vivasvaan Aditya Raj, Guido Roberts-Borsani, Axel Runnholm, Michael J. Rutkowski, Alberto Saldana-Lopez, Zahra Sattari, Claudia Scarlata, Kasper Borello Schmidt, Marko Shuntov, Harry Teplitz, Michele Trenti, Tommaso Treu, Benedetta Vulcani, Peter J. Watson, Xin Wang, Zhuyun Zhuang
Figure caption: A clumpy or interacting EELG from Par 28, displayed in the same layout as Figure 5. The disturbed morphology and extended emission in the 2D spectrum suggest merging components.
Paper: Parallel Application of Slitless Spectroscopy to Analyze Galaxy Evolution (PASSAGE): Survey Overview
Authors: Matthew A. Malkan, Vihang Mehta, Ayan Acharyya, Hollis B. Akins, Anahita Alavi, Hakim Atek, Ivano Baronchelli, Andrew J. Battisti, Kit Boyett, Marusa Bradac, Sean Tyler Bruton, Andrew J. Bunker, Adam J. Burgasser, Caitlin M. Casey, Nuo Chen, James Colbert, Y. Sophia Dai, Maximilien Franco, Clea Hannahs, Santosh Harish, Farhanul Hasan, Matthew J. Hayes, Alaina L. Henry, Mason Huberty, Tucker Jones, Jeyhan S. Kartaltepe, Keunho J. Kim, Nicha Leethochawalit, Jacob Levine, Sijia Li, Yu-Heng Lin, Yixiao Liu, Charlotte Mason, Daniel Masters, Henry Joy McCracken, Takahiro Morishita, Kalina V. Nedkova, Marc Rafelski, Vivasvaan Aditya Raj, Guido Roberts-Borsani, Axel Runnholm, Michael J. Rutkowski, Alberto Saldana-Lopez, Zahra Sattari, Claudia Scarlata, Kasper Borello Schmidt, Marko Shuntov, Harry Teplitz, Michele Trenti, Tommaso Treu, Benedetta Vulcani, Peter J. Watson, Xin Wang, Zhuyun Zhuang
Figure caption: PASSAGE is able to measure Lyα emission (LAE) with rest-frame EW > 50 Å in spectroscopically confirmed z > 8 galaxies. The lower left panel shows simulated z = 8.2 LAE spectra with mF115W = 27.5 (deep) with rest-frame EW(Lyα) of 30 Å (top row) and 50 Å (middle row). These are predicted to have clear Lyα detections. The bottom subpanel shows the simulated 1D spectra along with their noise for a range of EWs. These simulations are then compared with an actual PASSAGE detection of Lyα line emission. The lower right panels show the 2D and 1D F115W spectra for the object (visible in the direct images above), for both grism orientations, with the original spectral wavelength scales running along rows, and then along columns. Although these different orientations result in different nearby spectra, in both cases the Lyα line is independently detected at the same location and wavelength. The observed 2D spectrograms are 1﹩\mathop{.}\limits^{^{\prime\prime} }﹩4 high, while the simulated spectral images to the left are on approximately the same scale.