adsabs/AstroCLIMB huggingface dataset:
Paper: Molecular Gas in Major Mergers Hosting Dual and Single AGNs at <10 kpc Nuclear Separations
Authors: Makoto A. Johnstone, Ezequiel Treister, Franz E. Bauer, Chin-Shin Chang, Claudia Cicone, Michael J. Koss, Ignacio del Moral-Castro, Francisco Muller-Sanchez, George C. Privon, Claudio Ricci, Nick Scoville, Giacomo Venturi, Loreto Barcos-Muñoz, Lee Armus, Laura Blecha, Caitlin Casey, Julia Comerford, Aaron Evans, Taiki Kawamuro, Anne M. Medling, Hugo Messias, Neil Nagar, Alejandra Rojas, David Sanders, Benny Trakhtenbrot, Vivian U, Meg Urry
Figure caption: Surface density of nonrotating molecular gas mass (Σmol/M⊙/pc2)) with respect to MBH at both the SoI lower bound (a) and upper bound (b). Both axes are on a logarithmic scale. For systems where the SMBH SoI was smaller than the ALMA data cube’s beam size, we measure the molecular gas mass using a beam size aperture and present the value as an upper limit (shown as black arrows). We find that more-massive SMBHs have higher surface densities of nonrotating molecular gas in their SoIs.
Paper: Molecular Gas in Major Mergers Hosting Dual and Single AGNs at <10 kpc Nuclear Separations
Authors: Makoto A. Johnstone, Ezequiel Treister, Franz E. Bauer, Chin-Shin Chang, Claudia Cicone, Michael J. Koss, Ignacio del Moral-Castro, Francisco Muller-Sanchez, George C. Privon, Claudio Ricci, Nick Scoville, Giacomo Venturi, Loreto Barcos-Muñoz, Lee Armus, Laura Blecha, Caitlin Casey, Julia Comerford, Aaron Evans, Taiki Kawamuro, Anne M. Medling, Hugo Messias, Neil Nagar, Alejandra Rojas, David Sanders, Benny Trakhtenbrot, Vivian U, Meg Urry
Figure caption: Projected nuclear separation with respect to the molecular gas mass (Mmol/M⊙) within the SMBH SoI at both the SoI lower-bound (a) and upper-bound (b) estimates. The color scale indicates the fraction of the global molecular gas that lies within the SoI. Upper limits (shown as black arrows) are for unresolved SoI and/or 12CO nondetections. We find that, at lower projected nuclear separations, a higher fraction of the host galaxy’s molecular gas tends to lie within the SMBH SoI.
Paper: Molecular Gas in Major Mergers Hosting Dual and Single AGNs at <10 kpc Nuclear Separations
Authors: Makoto A. Johnstone, Ezequiel Treister, Franz E. Bauer, Chin-Shin Chang, Claudia Cicone, Michael J. Koss, Ignacio del Moral-Castro, Francisco Muller-Sanchez, George C. Privon, Claudio Ricci, Nick Scoville, Giacomo Venturi, Loreto Barcos-Muñoz, Lee Armus, Laura Blecha, Caitlin Casey, Julia Comerford, Aaron Evans, Taiki Kawamuro, Anne M. Medling, Hugo Messias, Neil Nagar, Alejandra Rojas, David Sanders, Benny Trakhtenbrot, Vivian U, Meg Urry
Figure caption: MBH with respect to nonrotating molecular gas mass (Mmol/M⊙) within the SMBH SoI at both the SoI lower bound (a) and upper bound (b). Both axes are on a logarithmic scale. Upper limits (shown as black arrows) are for unresolved SoI and/or 12CO nondetections. We find that larger SMBH masses correlate with larger molecular gas reservoirs within the SoI.
Paper: Molecular Gas in Major Mergers Hosting Dual and Single AGNs at <10 kpc Nuclear Separations
Authors: Makoto A. Johnstone, Ezequiel Treister, Franz E. Bauer, Chin-Shin Chang, Claudia Cicone, Michael J. Koss, Ignacio del Moral-Castro, Francisco Muller-Sanchez, George C. Privon, Claudio Ricci, Nick Scoville, Giacomo Venturi, Loreto Barcos-Muñoz, Lee Armus, Laura Blecha, Caitlin Casey, Julia Comerford, Aaron Evans, Taiki Kawamuro, Anne M. Medling, Hugo Messias, Neil Nagar, Alejandra Rojas, David Sanders, Benny Trakhtenbrot, Vivian U, Meg Urry
Figure caption: Aperture radius with respect to nonrotating molecular gas mass (Mmol/M⊙) at both the SoI lower bound (a) and upper bound (b). Both axes are on a logarithmic scale. Upper limits (shown as black arrows) are for unresolved SoI and/or 12CO nondetections. The black dashed line indicates a uniform 3σ mass distribution. No significant trend is observed, demonstrating that the MBH correlation in Figure 9 is not a product of differing aperture sizes.
Paper: Molecular Gas in Major Mergers Hosting Dual and Single AGNs at <10 kpc Nuclear Separations
Authors: Makoto A. Johnstone, Ezequiel Treister, Franz E. Bauer, Chin-Shin Chang, Claudia Cicone, Michael J. Koss, Ignacio del Moral-Castro, Francisco Muller-Sanchez, George C. Privon, Claudio Ricci, Nick Scoville, Giacomo Venturi, Loreto Barcos-Muñoz, Lee Armus, Laura Blecha, Caitlin Casey, Julia Comerford, Aaron Evans, Taiki Kawamuro, Anne M. Medling, Hugo Messias, Neil Nagar, Alejandra Rojas, David Sanders, Benny Trakhtenbrot, Vivian U, Meg Urry
Figure caption: Global molecular gas mass with respect to projected nuclear separation. Gas masses are reported for both αCO = 0.6 M⊙ (K km s−1 pc−2)−1 and αCO = 4.6 M⊙ (K km s−1 pc−2)−1, but error bars assume αCO = 0.6 M⊙ (K km s−1 pc−2)−1. No significant trend is observed, suggesting that the global supply of molecular gas in the host galaxy does not significantly evolve in the final stages of major mergers.
Paper: Molecular Gas in Major Mergers Hosting Dual and Single AGNs at <10 kpc Nuclear Separations
Authors: Makoto A. Johnstone, Ezequiel Treister, Franz E. Bauer, Chin-Shin Chang, Claudia Cicone, Michael J. Koss, Ignacio del Moral-Castro, Francisco Muller-Sanchez, George C. Privon, Claudio Ricci, Nick Scoville, Giacomo Venturi, Loreto Barcos-Muñoz, Lee Armus, Laura Blecha, Caitlin Casey, Julia Comerford, Aaron Evans, Taiki Kawamuro, Anne M. Medling, Hugo Messias, Neil Nagar, Alejandra Rojas, David Sanders, Benny Trakhtenbrot, Vivian U, Meg Urry
Figure caption:                         Same as Figure 4 for a single AGN. The AGN position is also overlaid as a black star. The upper bound of non-AGN SMBH’s SoI is overlaid as a black circle in the top right.
Paper: Discovery of 79 δ Scuti Stars in NGC 3532 Suggests a Decrease of Pulsator Occurrence with Age
Authors: Ian Berry, Daniel Huber, Yaguang Li, Daniel Hey, Timothy R. Bedding, Simon J. Murphy
Figure caption: Left: dereddened Gaia color–magnitude diagram (CMD) of NGC 3532. Color-mapped points are stars with a Gaia vbroad measurement, and gray points have no vbroad measurement. Star markers with red outlines are δ Scuti pulsators, while circular points are nonpulsators. Gray pluses are stars we did not search. Furthermore we plot MIST isochrones with age 300 Myr and [Fe/H] = −0.07 dex. The dotted isochrone is a nonrotating model, and the solid isochrone is a rotating model at 40% critical rotation speed. An empirically derived red instability strip (IS) edge from K. Gootkin et al. (2024) is shown as the dashed magenta line. Right: as in left except in ﹩{\mathrm{log}}L﹩ versus Teff space. Luminosities and Teff values come from the TIC catalog (K. G. Stassun et al. 2019). The magenta lines now show the empirically derived IS bounds from S. J. Murphy et al. (2019).
Paper: Discovery of 79 δ Scuti Stars in NGC 3532 Suggests a Decrease of Pulsator Occurrence with Age
Authors: Ian Berry, Daniel Huber, Yaguang Li, Daniel Hey, Timothy R. Bedding, Simon J. Murphy
Figure caption: Stacked amplitude spectra of all 79 δ Scuti stars in NGC 3532. Darker colors denote larger amplitudes. Stars are ordered by Gaia GBP − GRP, with bluest stars on top. The dashed red line marks 5 day−1, which is commonly used as the boundary between δ Scuti pulsations and other sources of low-frequency variability (e.g., G. Handler & R. R. Shobbrook 2002; M. Hareter et al. 2010; S. J. Murphy et al. 2019). Each amplitude spectrum is labeled with its corresponding star and color (without dereddening).
Paper: Discovery of 79 δ Scuti Stars in NGC 3532 Suggests a Decrease of Pulsator Occurrence with Age
Authors: Ian Berry, Daniel Huber, Yaguang Li, Daniel Hey, Timothy R. Bedding, Simon J. Murphy
Figure caption: Example amplitude spectra of three δ Scuti stars in NGC 3532, from aperture photometry (black) and PSF photometry (red). The stars are ordered by Gaia vbroad, and the TIC IDs and Gaia GBP − GRP are provided.
Paper: Discovery of 79 δ Scuti Stars in NGC 3532 Suggests a Decrease of Pulsator Occurrence with Age
Authors: Ian Berry, Daniel Huber, Yaguang Li, Daniel Hey, Timothy R. Bedding, Simon J. Murphy
Figure caption: Scatter plot showing the log skewness of peak amplitudes in aperture and PSF photometry from TGLC. We apply two lower boundaries in log skewness, 0.75 for both aperture and PSF photometry. Points are color coded by the signal-to-noise ratio (SNR) of the highest peak in the periodogram. The gray dashed line is the 1:1 line.
Paper: How the External Medium Outside Prestellar Cores Affects Protostellar Growth: Variations in Accretion Rate and Evolution of Disks and Outflows
Authors: Shingo Nozaki, Masahiro N. Machida
Figure caption: Density distributions on z = 0 (top) and y = 0 (bottom) planes for models B2H (left), B2 (middle) and B2L (right). Each panel shows the snapshot at Menv/M2BE,0 = 0.35. The white dotted and dashed–dotted circles in the bottom panels represent the positions of r = R1BE and r = R2BE.
Paper: How the External Medium Outside Prestellar Cores Affects Protostellar Growth: Variations in Accretion Rate and Evolution of Disks and Outflows
Authors: Shingo Nozaki, Masahiro N. Machida
Figure caption: The initial density profile in the radial direction for each model. The gray dotted and dashed–dotted lines represent 1 and 2 times the critical Bonnor–Ebert radius, corresponding to R1BE = 2.9 × 10−2 pc and R2BE = 5.7 × 10−2 pc. The color maps are the two-dimensional initial density slice in the y = 0 plane for the models B2H and B2L. The white dotted and dashed–dotted circles in the color maps indicate the positions of r = R1BE and r = R2BE.
Paper: Hyperaccretion-driven Relativistic Jets from Massive Collapsars in Active Galactic Nucleus Disks
Authors: Yun-Feng Wei, Tong Liu, Bao-Quan Huang
Figure caption: X-ray afterglow light curves of AGN GRBs with different progenitors. The black, red, and blue curves correspond to the cases of progenitors with metallicities of Z/Z⊙ = 0, 0.01, and 1, respectively. The solid, dashed, and dotted lines represent the progenitor masses of Mpro/M⊙ = 20, 30, and 40, respectively. The SMBH mass is 106M⊙. In panels (a) and (b), the radial locations from the SMBH are 104Rg and 105Rg, respectively.
Paper: Hyperaccretion-driven Relativistic Jets from Massive Collapsars in Active Galactic Nucleus Disks
Authors: Yun-Feng Wei, Tong Liu, Bao-Quan Huang
Figure caption: Same as Figure 5 but for an SMBH mass of 107M⊙. In panels (a) and (b), the radial locations from the SMBH are 103Rg and 104Rg, respectively.
Paper: Hyperaccretion-driven Relativistic Jets from Massive Collapsars in Active Galactic Nucleus Disks
Authors: Yun-Feng Wei, Tong Liu, Bao-Quan Huang
Figure caption: Same as Figure 5, but the SMBH mass is 108M⊙ and the radial locations from the SMBH is 103Rg.
Paper: Hyperaccretion-driven Relativistic Jets from Massive Collapsars in Active Galactic Nucleus Disks
Authors: Yun-Feng Wei, Tong Liu, Bao-Quan Huang
Figure caption: Same as Figure 9, but the SMBH mass is 108M⊙. In panel (a), the radial locations from the SMBH is 103Rg.
Paper: Hyperaccretion-driven Relativistic Jets from Massive Collapsars in Active Galactic Nucleus Disks
Authors: Yun-Feng Wei, Tong Liu, Bao-Quan Huang
Figure caption: Same as Figure 5 but for the EP case. The SMBH mass is 107M⊙. In panels (a) and (b), the radial locations from the SMBH are 103Rg and 104Rg, respectively.
Paper: Hyperaccretion-driven Relativistic Jets from Massive Collapsars in Active Galactic Nucleus Disks
Authors: Yun-Feng Wei, Tong Liu, Bao-Quan Huang
Figure caption: Same as Figure 9, but the SMBH mass is 107M⊙. In panels (a) and (b), the radial locations from the SMBH are 103Rg and 104Rg, respectively.
Paper: ODIN: Probing the LAE Lyα Luminosity Function across Cosmic Time and Different Environments
Authors: Gautam Nagaraj, Robin Ciardullo, Caryl Gronwall, Vandana Ramakrishnan, Kyoung-Soo Lee, Eric Gawiser, Nicole Firestone, Govind Ramgopal, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, F. J. Castander, T. Claybaugh, A. Cuceu, A. de la Macorra, Arjun Dey, Biprateep Dey, P. Doel, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, H. K. Herrera-Alcantar, K. Honscheid, M. Ishak, R. Kehoe, D. Kirkby, T. Kisner, A. Kremin, M. Landriau, L. Le Guillou, M. E. Levi, C. Magneville, M. Manera, P. Martini, A. Meisner, R. Miquel, J. Moustakas, N. Palanque-Delabrouille, F. Prada, I. Pérez-Ràfols, G. Rossi, L. Samushia, E. Sanchez, D. Schlegel, M. Schubnell, H. Seo, J. Silber, D. Sprayberry, G. Tarlé, F. Valdes, B. A. Weaver, M. White, R. Zhou, H. Zou
Figure caption: The ODIN LAE Lyα luminosity functions at redshifts z ∼ 2.4 (left panel), z ∼ 3.1 (middle panel), and z ∼ 4.5 (right panel) compared to results in the literature. The curves (light blue, orange, and green) show the range (up to ∼3σ from the median) of our MCMC solutions; the gray shaded regions show where the corrections are greater than a factor of ∼2, either due to photometric incompleteness or foreground contamination. Our results agree with the literature at ﹩{\mathrm{log}}\,L({\rm{Ly}}\alpha )\lesssim 43﹩ but display lower values at high luminosities. This offset is due to our use of DESI spectroscopy to statistically determine the impact of interlopers on the bright end of the function; a conventional treatment of contamination for N419 and N501 (blue triangles) leads to a result completely in agreement with the literature. See Section 3.2 for a more detailed discussion.
Paper: ODIN: Probing the LAE Lyα Luminosity Function across Cosmic Time and Different Environments
Authors: Gautam Nagaraj, Robin Ciardullo, Caryl Gronwall, Vandana Ramakrishnan, Kyoung-Soo Lee, Eric Gawiser, Nicole Firestone, Govind Ramgopal, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, F. J. Castander, T. Claybaugh, A. Cuceu, A. de la Macorra, Arjun Dey, Biprateep Dey, P. Doel, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, H. K. Herrera-Alcantar, K. Honscheid, M. Ishak, R. Kehoe, D. Kirkby, T. Kisner, A. Kremin, M. Landriau, L. Le Guillou, M. E. Levi, C. Magneville, M. Manera, P. Martini, A. Meisner, R. Miquel, J. Moustakas, N. Palanque-Delabrouille, F. Prada, I. Pérez-Ràfols, G. Rossi, L. Samushia, E. Sanchez, D. Schlegel, M. Schubnell, H. Seo, J. Silber, D. Sprayberry, G. Tarlé, F. Valdes, B. A. Weaver, M. White, R. Zhou, H. Zou
Figure caption: Parametric and nonparametric fits to the z ∼ 4.5 (N673) Lyα emission-line luminosity function of ODIN LAEs. The panels are the same as in Figure 8. Relative to N419 and N501, these data probe higher luminosities and are more uncertain at the bright end, due to our poorer understanding of foreground contamination. Nevertheless, the luminosity function displays the same general behavior as those of the N419 and N501 LAEs.(The data used to create this figure are available in the online article.)(The data used to create this figure are available.)
Paper: ODIN: Probing the LAE Lyα Luminosity Function across Cosmic Time and Different Environments
Authors: Gautam Nagaraj, Robin Ciardullo, Caryl Gronwall, Vandana Ramakrishnan, Kyoung-Soo Lee, Eric Gawiser, Nicole Firestone, Govind Ramgopal, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, F. J. Castander, T. Claybaugh, A. Cuceu, A. de la Macorra, Arjun Dey, Biprateep Dey, P. Doel, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, H. K. Herrera-Alcantar, K. Honscheid, M. Ishak, R. Kehoe, D. Kirkby, T. Kisner, A. Kremin, M. Landriau, L. Le Guillou, M. E. Levi, C. Magneville, M. Manera, P. Martini, A. Meisner, R. Miquel, J. Moustakas, N. Palanque-Delabrouille, F. Prada, I. Pérez-Ràfols, G. Rossi, L. Samushia, E. Sanchez, D. Schlegel, M. Schubnell, H. Seo, J. Silber, D. Sprayberry, G. Tarlé, F. Valdes, B. A. Weaver, M. White, R. Zhou, H. Zou
Figure caption: Comparison of the Schechter fits for the LAE luminosity functions in protoclusters (blue) and the field (yellow) at each of the three ODIN redshifts (left: z ∼ 2.4, middle: z ∼ 3.1, right: z ∼ 4.5). The much greater (∼3σ) range of MCMC solutions for the protocluster luminosity functions reflects the relatively small number of LAEs found within these systems. In the bottom panels, we show the ratio of the protocluster to field luminosity functions in purple (with the faint lines showing ratios for the individual random realizations in the top panels). While the protocluster luminosity functions are universally elevated compared to the field, there are also some intriguing differences in the shape: faint protocluster LAEs appear to be suppressed relative to the field. At z ∼ 4.5, there is also a clear suppression of bright protocluster LAEs. If borne out by further data, this would suggest that environmental processing has begun, even in these non-relaxed systems.
Paper: ODIN: Probing the LAE Lyα Luminosity Function across Cosmic Time and Different Environments
Authors: Gautam Nagaraj, Robin Ciardullo, Caryl Gronwall, Vandana Ramakrishnan, Kyoung-Soo Lee, Eric Gawiser, Nicole Firestone, Govind Ramgopal, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, F. J. Castander, T. Claybaugh, A. Cuceu, A. de la Macorra, Arjun Dey, Biprateep Dey, P. Doel, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, H. K. Herrera-Alcantar, K. Honscheid, M. Ishak, R. Kehoe, D. Kirkby, T. Kisner, A. Kremin, M. Landriau, L. Le Guillou, M. E. Levi, C. Magneville, M. Manera, P. Martini, A. Meisner, R. Miquel, J. Moustakas, N. Palanque-Delabrouille, F. Prada, I. Pérez-Ràfols, G. Rossi, L. Samushia, E. Sanchez, D. Schlegel, M. Schubnell, H. Seo, J. Silber, D. Sprayberry, G. Tarlé, F. Valdes, B. A. Weaver, M. White, R. Zhou, H. Zou
Figure caption: The evolution of the Schechter parameters in and out of protoclusters, as found from the ODIN data of the extended COSMOS field. In the first three panels, we show the values of the faint-end slope, the characteristic luminosity, and the normalization parameter, with the protocluster fits in blue and the field results in yellow. In the last panel, we show the integrated number density of LAEs. Unsurprisingly, the LAE number densities within protoclusters are ∼0.5 dex higher than in the field. The slight trend for α to be flatter in protoclusters causes most of the differences in shape seen in Figure 14.
Paper: ODIN: Probing the LAE Lyα Luminosity Function across Cosmic Time and Different Environments
Authors: Gautam Nagaraj, Robin Ciardullo, Caryl Gronwall, Vandana Ramakrishnan, Kyoung-Soo Lee, Eric Gawiser, Nicole Firestone, Govind Ramgopal, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, F. J. Castander, T. Claybaugh, A. Cuceu, A. de la Macorra, Arjun Dey, Biprateep Dey, P. Doel, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, H. K. Herrera-Alcantar, K. Honscheid, M. Ishak, R. Kehoe, D. Kirkby, T. Kisner, A. Kremin, M. Landriau, L. Le Guillou, M. E. Levi, C. Magneville, M. Manera, P. Martini, A. Meisner, R. Miquel, J. Moustakas, N. Palanque-Delabrouille, F. Prada, I. Pérez-Ràfols, G. Rossi, L. Samushia, E. Sanchez, D. Schlegel, M. Schubnell, H. Seo, J. Silber, D. Sprayberry, G. Tarlé, F. Valdes, B. A. Weaver, M. White, R. Zhou, H. Zou
Figure caption: Schechter fits to the ODIN data showing cosmic evolution of the Lyα luminosity function. The increase in the total number of galaxies with redshift is consistent with the known strong evolution out to z ∼ 3. Our fits seem to suggest that this evolution continues to z ∼ 4.5, in conflict with the minimal evolution expected between 3 < z < 6 (M. Ouchi et al. 2020). However, the bulk of these differences are at the bright end, where the number of spectra available for understanding contamination is low for z ∼ 4.5. There is some evidence for a gradual flattening of the faint-end slope with redshift, but larger and/or deeper samples are needed to confirm this feature.
Paper: ODIN: Probing the LAE Lyα Luminosity Function across Cosmic Time and Different Environments
Authors: Gautam Nagaraj, Robin Ciardullo, Caryl Gronwall, Vandana Ramakrishnan, Kyoung-Soo Lee, Eric Gawiser, Nicole Firestone, Govind Ramgopal, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, F. J. Castander, T. Claybaugh, A. Cuceu, A. de la Macorra, Arjun Dey, Biprateep Dey, P. Doel, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, H. K. Herrera-Alcantar, K. Honscheid, M. Ishak, R. Kehoe, D. Kirkby, T. Kisner, A. Kremin, M. Landriau, L. Le Guillou, M. E. Levi, C. Magneville, M. Manera, P. Martini, A. Meisner, R. Miquel, J. Moustakas, N. Palanque-Delabrouille, F. Prada, I. Pérez-Ràfols, G. Rossi, L. Samushia, E. Sanchez, D. Schlegel, M. Schubnell, H. Seo, J. Silber, D. Sprayberry, G. Tarlé, F. Valdes, B. A. Weaver, M. White, R. Zhou, H. Zou
Figure caption: The range of N501 luminosity functions (covering ∼3σ uncertainties) with (red) and without (blue) error propagation from the completeness/purity curves. While it is clear that the uncertainties are much larger in the former case, we still predict a lower luminosity function (albeit less significantly) at the bright end compared to the literature (various points, with the same colors and markers as in the middle panel of Figure 11). This difference is likely due to our use of DESI spectroscopy for the statistical removal of contamination.
Paper: ODIN: Probing the LAE Lyα Luminosity Function across Cosmic Time and Different Environments
Authors: Gautam Nagaraj, Robin Ciardullo, Caryl Gronwall, Vandana Ramakrishnan, Kyoung-Soo Lee, Eric Gawiser, Nicole Firestone, Govind Ramgopal, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, F. J. Castander, T. Claybaugh, A. Cuceu, A. de la Macorra, Arjun Dey, Biprateep Dey, P. Doel, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, H. K. Herrera-Alcantar, K. Honscheid, M. Ishak, R. Kehoe, D. Kirkby, T. Kisner, A. Kremin, M. Landriau, L. Le Guillou, M. E. Levi, C. Magneville, M. Manera, P. Martini, A. Meisner, R. Miquel, J. Moustakas, N. Palanque-Delabrouille, F. Prada, I. Pérez-Ràfols, G. Rossi, L. Samushia, E. Sanchez, D. Schlegel, M. Schubnell, H. Seo, J. Silber, D. Sprayberry, G. Tarlé, F. Valdes, B. A. Weaver, M. White, R. Zhou, H. Zou
Figure caption: Comparison of the likelihood contours of α and ﹩{\mathrm{log}}\,{L}_{* }﹩ for LAEs in z = 2.4, 3.1, and 4.5 protoclusters (blue) and the field (yellow) as derived via the MCMC method. The panels show 1σ, 2σ, and 3σ contour levels in increasing transparency of the colors. The two sets of contours overlap in all three bands, meaning that at this time, we cannot confidently draw any conclusions about the effects of environment on the LAE luminosity function.
Paper: The Enhancement of Ion Heating in Kinetic, Antiparallel Reconnection in the Presence of a Flow Shear
Authors: Colby C. Haggerty, Derek Sikorski, Michael A. Shay, Tai D. Phan, Paul A. Cassak, Giulia Murtas, Prayash S. Pyakurel
Figure caption: Comparison between simulations (orange triangles) and predictions (multicolored solid lines) for the outflow velocity (top panel) and ion heating (bottom panel) as a function of inflowing flow shear speed. The different colors correspond to the predictions for different initial ion temperatures, as described in the legend, with the black–dark-orange dashed line having the same initial temperature as the simulations.