adsabs/AstroCLIMB huggingface dataset:
Paper: Phase Mixing of Propagating Alfvén Waves in a Single-fluid Partially Ionized Solar Plasma
Authors: M. McMurdo, I. Ballai, G. Verth, A. Alharbi, V. Fedun
Figure caption: The variation of the heating rate with the ionization degree of the plasma for the phase-mixed Alfvén waves with a wavelength of 400 km described by the P 4 profile. Heating rates associated with particular dissipative coefficients are shown by different colors. The horizontal black line shows the value of the heating rate of the quiet Sun equal to the average radiative losses of the chromosphere.
Paper: Phase Mixing of Propagating Alfvén Waves in a Single-fluid Partially Ionized Solar Plasma
Authors: M. McMurdo, I. Ballai, G. Verth, A. Alharbi, V. Fedun
Figure caption: Percentage change in the amplitude of Alfvén waves for six different ionization degrees (displayed in the top right of each panel) in terms of the wavelength of Alfvén waves, here in the range of 300–1100 km. The colors denote the same initial Alfvén wave profiles as before.
Paper: Phase Mixing of Propagating Alfvén Waves in a Single-fluid Partially Ionized Solar Plasma
Authors: M. McMurdo, I. Ballai, G. Verth, A. Alharbi, V. Fedun
Figure caption: A composite figure showing the formation height and temperature of various continua and spectral lines, taken from Vernazza et al. (1981), over which we plot the height and temperature range (shaded box) for which the heating rate produced by the phase mixing of Alfvén waves is larger than the radiative loses in the quiet chromosphere.
Paper: Early Planet Formation in Embedded Disks (eDisk). XII. Accretion Streamers, Protoplanetary Disk, and Outflow in the Class I Source Oph IRS 63
Authors: Christian Flores, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Shigehisa Takakuwa, Zhi-Yun Li, Zhe-Yu Daniel Lin, Merel L. R. van 't Hoff, Adele L. Plunkett, Yoshihide Yamato, Jinshi Sai (Insa Choi), Patrick M. Koch, Hsi-Wei Yen, Yuri Aikawa, Yusuke Aso, Itziar de Gregorio-Monsalvo, Miyu Kido, Woojin Kwon, Jeong-Eun Lee, Chang Won Lee, Leslie W. Looney, Alejandro Santamaría-Miranda, Rajeeb Sharma, Travis J. Thieme, Jonathan P. Williams, Ilseung Han, Suchitra Narayanan, Shih-Ping Lai
Figure caption: Four maps showing different aspects of the 12CO outflow emission. Panel (a) shows the peak intensity or moment 8 map. Panel (b) shows the moment 1 map in colors, obtained by integrated emission above 6σ, from channels at V LSR = −12.37 to −0.94 km s−1 and from V LSR = 4.78 to 17.48 km s−1. The map is also overlaid in black contours by the moment 0 map starting at 3σ, in steps of 8σ (1σ = 8 mJy beam−1 km s−1). In panel (c), we show two channels at V LSR = −2.21 km s−1 (blueshifted side) and V LSR = 6.05 km s−1 (redshifted side) to emphasize the complex shell-like structure of the outflow. Panel (d) is an overlay between redshifted outflow at V LSR = 4.78 km s−1 and the arc-like emission of C18O from channel at VLSR = 3.02 km s−1 (in black contours). The FOV in all maps is 26″ × 26″.
Paper: Early Planet Formation in Embedded Disks (eDisk). XII. Accretion Streamers, Protoplanetary Disk, and Outflow in the Class I Source Oph IRS 63
Authors: Christian Flores, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Shigehisa Takakuwa, Zhi-Yun Li, Zhe-Yu Daniel Lin, Merel L. R. van 't Hoff, Adele L. Plunkett, Yoshihide Yamato, Jinshi Sai (Insa Choi), Patrick M. Koch, Hsi-Wei Yen, Yuri Aikawa, Yusuke Aso, Itziar de Gregorio-Monsalvo, Miyu Kido, Woojin Kwon, Jeong-Eun Lee, Chang Won Lee, Leslie W. Looney, Alejandro Santamaría-Miranda, Rajeeb Sharma, Travis J. Thieme, Jonathan P. Williams, Ilseung Han, Suchitra Narayanan, Shih-Ping Lai
Figure caption: Integrated intensity maps of the molecules presented in this work. The emission goes from 1σ of the integrated intensity to the maximum value of the map. The color scales were stretched using an arcsinh function to emphasize faint structures. The 5σ contour of the continuum emission is plotted in red. For the 12CO molecule, the map size is 26″ × 26″ and the velocity integrations are from −12.37 to −0.94 km s−1 and from 5.40 to 17.48 km s−1. For 13CO and C18O, the map sizes are 20″ × 20″. The moment 0 maps for 13CO and C18O were integrated between −2.33 and 1.85 km s−1  and between 3.18 and 6.02 km s−1 and from 0.01 to 2.35 km s−1  and from 2.85 to 5.69 km s−1, respectively. For SO and H2CO, the maps sizes are 13″ × 13″. The velocity integrations are 0.18–5.52 km s−1 and 0.72–4.72 km s−1, respectively. Beam sizes are depicted in the lower left corner of the maps, according to Table 1. A horizontal bar of size 250 au is presented in the lower right corner of the C18O map. All maps are centered using the Gaussian fit to the continuum emission at the coordinates R.A. = 16:31:35.654 and decl. = −24:01:30.08.
Paper: Early Planet Formation in Embedded Disks (eDisk). XII. Accretion Streamers, Protoplanetary Disk, and Outflow in the Class I Source Oph IRS 63
Authors: Christian Flores, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Shigehisa Takakuwa, Zhi-Yun Li, Zhe-Yu Daniel Lin, Merel L. R. van 't Hoff, Adele L. Plunkett, Yoshihide Yamato, Jinshi Sai (Insa Choi), Patrick M. Koch, Hsi-Wei Yen, Yuri Aikawa, Yusuke Aso, Itziar de Gregorio-Monsalvo, Miyu Kido, Woojin Kwon, Jeong-Eun Lee, Chang Won Lee, Leslie W. Looney, Alejandro Santamaría-Miranda, Rajeeb Sharma, Travis J. Thieme, Jonathan P. Williams, Ilseung Han, Suchitra Narayanan, Shih-Ping Lai
Figure caption: Comparison between the continuum (contours) and molecular emission of 13CO, C18O, SO, and H2CO (colors), respectively. The continuum emission is plotted at contour levels of 6σ, 20σ, and 50σ. The beam size of the continuum is 0.″034  ×  0.″025, while the beam size of the gas is ∼10 times larger. The top row shows the moment 0 maps, while the bottom row shows the moment 1 maps. The velocities of the moment 1 maps are corrected for v sys (i.e., we subtracted v sys = 2.8 km s−1 to the map). The FOV of all the maps is 5″ × 5″.
Paper: Early Planet Formation in Embedded Disks (eDisk). XII. Accretion Streamers, Protoplanetary Disk, and Outflow in the Class I Source Oph IRS 63
Authors: Christian Flores, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Shigehisa Takakuwa, Zhi-Yun Li, Zhe-Yu Daniel Lin, Merel L. R. van 't Hoff, Adele L. Plunkett, Yoshihide Yamato, Jinshi Sai (Insa Choi), Patrick M. Koch, Hsi-Wei Yen, Yuri Aikawa, Yusuke Aso, Itziar de Gregorio-Monsalvo, Miyu Kido, Woojin Kwon, Jeong-Eun Lee, Chang Won Lee, Leslie W. Looney, Alejandro Santamaría-Miranda, Rajeeb Sharma, Travis J. Thieme, Jonathan P. Williams, Ilseung Han, Suchitra Narayanan, Shih-Ping Lai
Figure caption: Large-scale maps of 13CO. The left panel shows the peak intensity map (moment 8) in units of mJy beam−1. The right panel shows the velocity structure (moment 1 map) centered at V sys = 2.8 km s−1. The moment 1 map was obtained by integrating emission above 22.5 mJy beam−1 (5 times the rms). The integrated intensity (moment 0) is overlaid in black contours starting at 1σ (1σ = 4.7 mJy beam−1 km s−1) with a step of 6σ. Both maps show the connection of a large-scale structure (>5″) to a compact (∼2″) disk-like structure. The FOV in both maps is 23″ × 23″.
Paper: Early Planet Formation in Embedded Disks (eDisk). XII. Accretion Streamers, Protoplanetary Disk, and Outflow in the Class I Source Oph IRS 63
Authors: Christian Flores, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Shigehisa Takakuwa, Zhi-Yun Li, Zhe-Yu Daniel Lin, Merel L. R. van 't Hoff, Adele L. Plunkett, Yoshihide Yamato, Jinshi Sai (Insa Choi), Patrick M. Koch, Hsi-Wei Yen, Yuri Aikawa, Yusuke Aso, Itziar de Gregorio-Monsalvo, Miyu Kido, Woojin Kwon, Jeong-Eun Lee, Chang Won Lee, Leslie W. Looney, Alejandro Santamaría-Miranda, Rajeeb Sharma, Travis J. Thieme, Jonathan P. Williams, Ilseung Han, Suchitra Narayanan, Shih-Ping Lai
Figure caption: Large-scale maps of C18O. The left panel shows the peak intensity map (moment 8) in units of mJy beam−1. The right panel shows the velocity structure (moment 1 map) centered at V sys = 2.8 km s−1. The moment 1 map was obtained by integrating emission above 15 mJy beam−1(5 times the rms). The integrated intensity (moment 0) is overlaid in black contours starting at 1σ (1σ = 2.3 mJy beam−1 km s−1) with a step of 6σ. The FOV in both maps is 23″ × 23″.
Paper: Early Planet Formation in Embedded Disks (eDisk). XII. Accretion Streamers, Protoplanetary Disk, and Outflow in the Class I Source Oph IRS 63
Authors: Christian Flores, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Shigehisa Takakuwa, Zhi-Yun Li, Zhe-Yu Daniel Lin, Merel L. R. van 't Hoff, Adele L. Plunkett, Yoshihide Yamato, Jinshi Sai (Insa Choi), Patrick M. Koch, Hsi-Wei Yen, Yuri Aikawa, Yusuke Aso, Itziar de Gregorio-Monsalvo, Miyu Kido, Woojin Kwon, Jeong-Eun Lee, Chang Won Lee, Leslie W. Looney, Alejandro Santamaría-Miranda, Rajeeb Sharma, Travis J. Thieme, Jonathan P. Williams, Ilseung Han, Suchitra Narayanan, Shih-Ping Lai
Figure caption: Left: dust continuum image with robust parameter R = 0.0. The beam of size 0.″034 × 0.″025 is represented by a white ellipse in the lower left corner. A 20 au scale bar is shown for reference in the lower right corner. Right: average radial intensity profile. Color lines represent radial profiles obtained for images with different robust parameters. Two ring-like structures are visually identified at distances of 0.″16 and 0.″34, whose positions are in agreement with results from Segura-Cox et al. (2020).
Paper: Early Planet Formation in Embedded Disks (eDisk). XII. Accretion Streamers, Protoplanetary Disk, and Outflow in the Class I Source Oph IRS 63
Authors: Christian Flores, Nagayoshi Ohashi, John J. Tobin, Jes K. Jørgensen, Shigehisa Takakuwa, Zhi-Yun Li, Zhe-Yu Daniel Lin, Merel L. R. van 't Hoff, Adele L. Plunkett, Yoshihide Yamato, Jinshi Sai (Insa Choi), Patrick M. Koch, Hsi-Wei Yen, Yuri Aikawa, Yusuke Aso, Itziar de Gregorio-Monsalvo, Miyu Kido, Woojin Kwon, Jeong-Eun Lee, Chang Won Lee, Leslie W. Looney, Alejandro Santamaría-Miranda, Rajeeb Sharma, Travis J. Thieme, Jonathan P. Williams, Ilseung Han, Suchitra Narayanan, Shih-Ping Lai
Figure caption: Integrated intensity of the SO emission to highlight the spiral pattern. The moment 0 map was generated using only emission above 3σ. The spirals S1, S2, and S3 depict the spiral patterns connecting with the ring-like feature on the north, east, and south, respectively. The continuum is shown in black contours at 6σ, 20σ, 40σ, and 150σ. The image has an FOV of 5.″5 × 5.″5.
Paper: Spectro-polarimetric Properties of Sunquake Sources in X1.5 Flare and Evidence for Electron and Proton Beam Impacts
Authors: Alexander G. Kosovichev, Viacheslav M. Sadykov, John T. Stefan
Figure caption: Source 1a: (a) image of the Fe I 6173 Å line continuum intensity time difference during the flare impact; (b) image of the line-core intensity time difference during the flare impact; (c) the temporal behavior of the line continuum (solid curve) and core (dashed curve) averaged over the black box in panels (a) and (b); (d) variations of the line profile at different time moments before, during, and after the impact; (e) the corresponding variations of Stokes I, Q, U, and V line profiles.
Paper: Spectro-polarimetric Properties of Sunquake Sources in X1.5 Flare and Evidence for Electron and Proton Beam Impacts
Authors: Alexander G. Kosovichev, Viacheslav M. Sadykov, John T. Stefan
Figure caption: The same as in Figure 6 for Source 2b.
Paper: Spectro-polarimetric Properties of Sunquake Sources in X1.5 Flare and Evidence for Electron and Proton Beam Impacts
Authors: Alexander G. Kosovichev, Viacheslav M. Sadykov, John T. Stefan
Figure caption: The photospheric flare impacts observed by the HMI instrument around 13:56:20 UT (Source 1) and 13:57:50 UT (Source 2). Panels (a) and (c) show the relative continuum intensity enhancements during 45 s of the impacts; panels (b) and (d) show the line-of-sight magnetograms during the flare impacts. The contour lines show the corresponding Doppler velocity signals for 3, 4, 5, 6, and 7 km s−1. Solid lines show the positive (redshifted) velocity, and dashed lines show the negative velocity.
Paper: Spectro-polarimetric Properties of Sunquake Sources in X1.5 Flare and Evidence for Electron and Proton Beam Impacts
Authors: Alexander G. Kosovichev, Viacheslav M. Sadykov, John T. Stefan
Figure caption: The vertical electric currents at around (a) 13:57:00 UT (Source 1) and (b) 13:58:30 UT (Source 2). The overlaid contours of the Doppler velocity signals are the same as in Figure 4. (c) The magnetic field lines reconstructed in the NLFFF approximation from the HMI 720 s vector magnetograms centered at 13:54 UT using the GX Simulator (Nita et al. 2023; the image is courtesy of G. Nita).
Paper: Spectro-polarimetric Properties of Sunquake Sources in X1.5 Flare and Evidence for Electron and Proton Beam Impacts
Authors: Alexander G. Kosovichev, Viacheslav M. Sadykov, John T. Stefan
Figure caption: The time–distance diagrams obtained by the angular averaging of the frequency-filtered Dopplergrams with the central points located in the Source 1 (a) and Source 2 (b) areas. The angular averaging is performed for the north-oriented quadrant.
Paper: Spectro-polarimetric Properties of Sunquake Sources in X1.5 Flare and Evidence for Electron and Proton Beam Impacts
Authors: Alexander G. Kosovichev, Viacheslav M. Sadykov, John T. Stefan
Figure caption: The evolution of the Stokes Q, U, and V profiles in the flare sources before and during the Stokes I emission peaks.
Paper: Spectro-polarimetric Properties of Sunquake Sources in X1.5 Flare and Evidence for Electron and Proton Beam Impacts
Authors: Alexander G. Kosovichev, Viacheslav M. Sadykov, John T. Stefan
Figure caption: The soft X-ray flare emission in the energy band 1.5–12 keV observed by the GOES satellite (red), and the hard X-ray emission in the energy bands 19–81 keV and 82–322 keV (blue) observed by the KONUS/WIND instrument (Lysenko et al. 2022).
Paper: Spectro-polarimetric Properties of Sunquake Sources in X1.5 Flare and Evidence for Electron and Proton Beam Impacts
Authors: Alexander G. Kosovichev, Viacheslav M. Sadykov, John T. Stefan
Figure caption: The same as in Figure 6 for Source 2a.
Paper: Spectro-polarimetric Properties of Sunquake Sources in X1.5 Flare and Evidence for Electron and Proton Beam Impacts
Authors: Alexander G. Kosovichev, Viacheslav M. Sadykov, John T. Stefan
Figure caption: The same as in Figure 6 for Source 1b.
Paper: Environmental Impacts on the Rest-frame UV Size and Morphology of Star-forming Galaxies at z ∼ 2
Authors: Abdurrahman Naufal, Yusei Koyama, Rhythm Shimakawa, Tadayuki Kodama
Figure caption: The stellar mass–half-light radius relation of HAEs in our sample. Semitransparent purple (gray) triangles (circles) are HAEs in protoclusters (field), while their solid counterparts are binned according to the stellar mass. White-filled triangles (circles) are the stacked galaxy of the same mass bin for protocluster (field) HAEs, multiplied by the correction factor (see the text). The red line denotes the derived fit for field galaxies (Equation (9)) to compare with the results from Van Der Wel et al. (2014) shown by dashed and dotted lines for LTGs and ETGs, respectively. We did not find a significant difference between protoclusters and field samples in either mass bin.
Paper: Environmental Impacts on the Rest-frame UV Size and Morphology of Star-forming Galaxies at z ∼ 2
Authors: Abdurrahman Naufal, Yusei Koyama, Rhythm Shimakawa, Tadayuki Kodama
Figure caption: The distribution of ﹩\mathrm{log}{r}_{S\mathrm{\unicode{x000E9}rsic}}﹩ to the one predicted by Equation (9). We divide the samples into three SFR bins as shown in the bottom three panels. In each panel, the distribution for the protocluster (field) sample is represented by the purple (gray) histogram. Each panel includes galaxies within SFR–M ⋆ ranges as illustrated in Figure 1. For all subsets, we do not find significant differences in size at fixed stellar mass according to Anderson–Darling tests.
Paper: Environmental Impacts on the Rest-frame UV Size and Morphology of Star-forming Galaxies at z ∼ 2
Authors: Abdurrahman Naufal, Yusei Koyama, Rhythm Shimakawa, Tadayuki Kodama
Figure caption: Plot summarizing various studies on star-forming galaxies in different environments (Peter et al. 2007; Lani et al. 2013; Cebrián & Trujillo 2014; Allen et al. 2015, 2016; Tran et al. 2017; Matharu et al. 2019). r cluster/r field is the ratio of the size of star-forming galaxies in clusters to those in the field at fixed stellar mass (if such value is unreported, we use the ratio of the median of the distributions). Our work provides four data points at z ∼ 2 (cyan, pink, gold, and slate blue stars for individual protoclusters; purple star for all protoclusters). We do not find a significant difference in size at fixed stellar mass between protocluster and field HAEs at z ∼ 2.
Paper: Environmental Impacts on the Rest-frame UV Size and Morphology of Star-forming Galaxies at z ∼ 2
Authors: Abdurrahman Naufal, Yusei Koyama, Rhythm Shimakawa, Tadayuki Kodama
Figure caption: Diagram showing the protocluster HAEs (purple triangles) and field HAEs (gray circles) in the Gini–M 20 plane. The dotted line represents the zero line of the bulge statistics as it segregates disk-dominated (below, negative bulge statistics) and bulge-dominated statistics (above, positive bulge statistics galaxies. Similarly, the dashed line represented the zero line of the merger statistics above which the merger candidates lie (positive merger statistics; Snyder et al. 2015a; Rodriguez-Gomez et al. 2019). As seen here, most HAEs in our sample are consistent with a disk-dominated profile, but also a significant fraction of them have peculiar morphologies that possibly indicate clumpy or merging systems.
Paper: Environmental Impacts on the Rest-frame UV Size and Morphology of Star-forming Galaxies at z ∼ 2
Authors: Abdurrahman Naufal, Yusei Koyama, Rhythm Shimakawa, Tadayuki Kodama
Figure caption: Histogram of morphology indicators of protocluster (purple) and field (gray) HAEs. From top left to bottom right: Sérsic half-light radius, Sérsic index, concentration, asymmetry, Gini, M 20, and two statistics derived from Gini-M 20: bulge factor and merger statistics. Purple dashed (black dotted) vertical lines denote the median of the protocluster (field) sample. In each panel, we show the Anderson–Darling coefficients, where AD > 1.961 corresponds to p < 0.05 significance. We find significant differences in Gini and the two Gini-M 20 statistics.
Paper: Environmental Impacts on the Rest-frame UV Size and Morphology of Star-forming Galaxies at z ∼ 2
Authors: Abdurrahman Naufal, Yusei Koyama, Rhythm Shimakawa, Tadayuki Kodama
Figure caption: Each panel shows a plot of a morphology statistic compared with stellar mass ﹩\mathrm{log}{M}_{\star }/{M}_{\odot }﹩. The stellar mass bins are the same as in Figure 5. The black-bordered symbol represents the median of each bin. The error bars are within the 16th and 84th percentiles of the bootstrapped median distribution. Only the stellar mass–size relation (top left) is a statistically significant correlation according to the Spearman test (p < 0.05).
Paper: Environmental Impacts on the Rest-frame UV Size and Morphology of Star-forming Galaxies at z ∼ 2
Authors: Abdurrahman Naufal, Yusei Koyama, Rhythm Shimakawa, Tadayuki Kodama
Figure caption: Similar to Figure 10, but each panel shows a plot of a morphology statistic compared with the offset from an SFMS ﹩{\rm{\Delta }}\mathrm{log}\,\mathrm{SFR}﹩. The three bins correspond to below the SFMS, on the SFMS, and the above SFMS samples. Asymmetry, Gini, and merger statistics are positively correlated with ﹩{\rm{\Delta }}\mathrm{log}\,\mathrm{SFR}﹩ (p < 0.05).
Paper: Environmental Impacts on the Rest-frame UV Size and Morphology of Star-forming Galaxies at z ∼ 2
Authors: Abdurrahman Naufal, Yusei Koyama, Rhythm Shimakawa, Tadayuki Kodama
Figure caption: Radial profiles of stacked field HAEs (solid gray line) and stacked protocluster HAEs (solid purple line). The shaded regions are uncertainties of the stacked profile from bootstrapping. The radial profiles of best-fitting Sérsic models are shown as dashed lines and the PSF is shown as the black dotted line.
Paper: Environmental Impacts on the Rest-frame UV Size and Morphology of Star-forming Galaxies at z ∼ 2
Authors: Abdurrahman Naufal, Yusei Koyama, Rhythm Shimakawa, Tadayuki Kodama
Figure caption: An example figure produced by STATMORPH of the morphological measurement of an HAE in CC 22. The properties relevant to Sérsic fitting, asymmetry, Gini, M 20, MID, and shape asymmetry are shown. The two bottom right panels, showing MID and shape asymmetry, are not discussed in this work.
Paper: A Spectroscopic Survey of Lyα Emitters and Lyα Luminosity Function at Redshifts 3.7 and 4.8
Authors: Weiyang Liu, Linhua Jiang
Figure caption: Lyα LFs at z ∼ 4.8. The red points with error bars represent the binned LF of the z ∼ 4.8 LAE sample. The vertical error bars denote the 1σ Poisson error and the horizontal bars indicate the bin size of ﹩{\rm{\Delta }}\mathrm{log}L=0.2﹩ dex. The black solid line is the best-fit LF with the Schechter function and α fixed to −1.5 for the z ∼ 4.8 LAE sample. Lyα LFs at similar redshifs in the literature are also shown (Shioya+09: Shioya et al. 2009; Cassata+11: Cassata et al. 2011; Zheng+13: Zheng et al. 2013; Drake+17: Drake et al. 2017; Sobral+18: Sobral et al. 2018; Herenz+19: Herenz et al. 2019). Dashed and solid lines indicate Lyα LFs calculated from photometric LAE samples and spectroscopically confirmed LAE samples, respectively.
Paper: A Spectroscopic Survey of Lyα Emitters and Lyα Luminosity Function at Redshifts 3.7 and 4.8
Authors: Weiyang Liu, Linhua Jiang
Figure caption: Lyα LFs at z ∼ 3.7. The red points with error bars represent the binned LF of the z ∼ 3.7 LAE sample. The vertical error bars denote the 1σ Poisson error and the horizontal bars indicate the bin size of ﹩{\rm{\Delta }}\mathrm{log}L=0.2﹩ dex. The black solid line is the best-fit LF with the Schechter function and α fixed to −1.5 for the z ∼ 3.7 LAE sample. Lyα LFs at similar redshifs in the literature are also shown (Ouchi+08: Ouchi et al. 2008; Cassata+11: Cassata et al. 2011; Drake+17: Drake et al. 2017; Sobral+18: Sobral et al. 2018; Herenz+19: Herenz et al. 2019; Zhang+21: Zhang et al. 2021). Dashed and solid lines indicate Lyα LFs calculated from photometric LAE samples and spectroscopically confirmed LAE samples, respectively.
Paper: A Spectroscopic Survey of Lyα Emitters and Lyα Luminosity Function at Redshifts 3.7 and 4.8
Authors: Weiyang Liu, Linhua Jiang
Figure caption: Lyα LF at several redshifts based on spectroscopically confirmed LAE samples. z ∼ 3.1: Guo et al. (2020); z ∼ 3.7: this work; z ∼ 4.8: this work; z ∼ 5.7: Zheng et al. (in preparation); z ∼ 6.6: Ning et al. (2022). These lines are the best-fit Schechter functions.
Paper: A Spectroscopic Survey of Lyα Emitters and Lyα Luminosity Function at Redshifts 3.7 and 4.8
Authors: Weiyang Liu, Linhua Jiang
Figure caption: Total completeness fraction (combining source detection, target selection, and spectroscopic observations) in different subfields as a function of the Lyα luminosity and redshift. The three contours represent the fractions of 10%, 50%, and 70% in the upper panel, and 10%, 30%, and 50% in the lower panel. The red points with error bars represent the LAEs in our samples.
Paper: A Spectroscopic Survey of Lyα Emitters and Lyα Luminosity Function at Redshifts 3.7 and 4.8
Authors: Weiyang Liu, Linhua Jiang
Figure caption: Likelihood contours in the ﹩{\phi }_{\mathrm{Ly}\alpha }^{* }-{L}_{\mathrm{Ly}\alpha }^{* }﹩ parameter space for the two LAE samples at z ∼ 3.7 (blue) and z ∼ 4.8 (red). The blue and red dots show the best-fit ﹩{\phi }_{\mathrm{Ly}\alpha }^{* }﹩ and ﹩{L}_{\mathrm{Ly}\alpha }^{* }﹩. The solid and dashed lines represent 1σ (68%) and 2σ (95%) confidence regions, respectively.
Paper: A Spectroscopic Survey of Lyα Emitters and Lyα Luminosity Function at Redshifts 3.7 and 4.8
Authors: Weiyang Liu, Linhua Jiang
Figure caption: Distribution of the UV slope β for z ∼ 3.7 LAE sample. The dashed line represents the best-fit Gaussian distribution with an average β = −1.72 and σ  β  = 0.80.