adsabs/AstroCLIMB huggingface dataset:
Paper: Detecting Multiplanetary Systems with Gravitational Microlensing and the Roman Space Telescope
Authors: Hossein Fatheddin, Sedighe Sajadian
Figure caption: Panels (a) and (b) show the change in the mean magnification and caustic area of the second planet with respect to its separation (s 31). Figure (c) and (d) show the change in the mean magnification and caustic area of the second planet with respect to its mass ratio (q 31).
Paper: Detecting Multiplanetary Systems with Gravitational Microlensing and the Roman Space Telescope
Authors: Hossein Fatheddin, Sedighe Sajadian
Figure caption: Parameters of a Triple Lens system. The three lenses are labeled as m 1, m 2, m 3 (where m 1 is the host star and m 2 and m 3 are the planets). The trajectory of the source is also illustrated. The coordinate system is centered on the host star.
Paper: Centimeter-sized Grains in the Compact Dust Ring around Very-low-mass Star CIDA 1
Authors: Jun Hashimoto, Hauyu Baobab Liu, Ruobing Dong, Beibei Liu, Takayuki Muto, Yuka Terada
Figure caption: The observed flux densities from CIDA 1, represented by circles, are compared to our models for interpretation. The flux densities used are listed above the separator line in Table 3. The flux uncertainties are explained in the table caption in Table 3. Left: the integrated flux densities from CIDA 1 are plotted on a logarithmic scale. Right: the flux density of the CIDA 1 inner disk is shown. In all panels, the blue, green, yellow, and pink lines correspond to our models for the dust emission from the inner disk, an embedded dust ring with ﹩{a}_{{\rm{\max }}}=25\,\mathrm{mm}﹩, a spatially compact embedded dust component with ﹩{a}_{{\rm{\max }}}=0.9\,\mathrm{mm}﹩, and an extended dust ring with ﹩{a}_{{\rm{\max }}}=0.55\,\mathrm{mm}﹩, respectively (refer to Table 4 for a summary of our model). The black lines represent the total flux densities of all model components.
Paper: Centimeter-sized Grains in the Compact Dust Ring around Very-low-mass Star CIDA 1
Authors: Jun Hashimoto, Hauyu Baobab Liu, Ruobing Dong, Beibei Liu, Takayuki Muto, Yuka Terada
Figure caption: Zoomed-in Ka-band image (0.″18 × 0.″16) superposed with contours of ALMA Band 7 image (54 mas × 37 mas; Pinilla et al. 2021). Contour levels are 17.1 μJy beam−1 (1σ) × [5, 15, 45]. The stellar position is marked by a black star. VLA and ALMA FITS images shown in this figure are available as data behind the figure (see Figure 1).
Paper: Centimeter-sized Grains in the Compact Dust Ring around Very-low-mass Star CIDA 1
Authors: Jun Hashimoto, Hauyu Baobab Liu, Ruobing Dong, Beibei Liu, Takayuki Muto, Yuka Terada
Figure caption: The inner disk component is explored in Q- and Ka-band data. Left: the CLEAN components. There is a CLEAN component with 4.2 μJy beam−1 in the central region of Q-band data in panel (a). Right: residual images with a specific mask on the ring region indicated by the dashed ellipse in Figure 1. The peak flux of the central region in both residual images is less than 1σ (Table 2).
Paper: Survey Operations for the Dark Energy Spectroscopic Instrument
Authors: Edward F. Schlafly, David Kirkby, David J. Schlegel, Adam D. Myers, Anand Raichoor, Kyle Dawson, Jessica Aguilar, Carlos Allende Prieto, Stephen Bailey, Segev BenZvi, Jose Bermejo-Climent, David Brooks, Axel de la Macorra, Arjun Dey, Peter Doel, Kevin Fanning, Andreu Font-Ribera, Jaime E. Forero-Romero, Juan García-Bellido, Satya Gontcho A Gontcho, Julien Guy, ChangHoon Hahn, Klaus Honscheid, Mustapha Ishak, Stéphanie Juneau, Robert Kehoe, Theodore Kisner, Anthony Kremin, Martin Landriau, Dustin A. Lang, James Lasker, Michael E. Levi, Christophe Magneville, Christopher J. Manser, Paul Martini, Aaron M. Meisner, Ramon Miquel, John Moustakas, Jeffrey A. Newman, Jundan Nie, Nathalie. Palanque-Delabrouille, Will J. Percival, Claire Poppett, Constance Rockosi, Ashley J. Ross, Graziano Rossi, Gregory Tarlé, Benjamin A. Weaver, Christophe Yèche, Rongpu Zhou
Figure caption: Schematic flow chart of DESI operations steps, running from planning for the night, through each night’s observations, and then through their reduction and updates to the MTL. Steps in the dashed box are optional and may be skipped temporarily if systems are not available. See Section 5.1 for details.
Paper: Survey Operations for the Dark Energy Spectroscopic Instrument
Authors: Edward F. Schlafly, David Kirkby, David J. Schlegel, Adam D. Myers, Anand Raichoor, Kyle Dawson, Jessica Aguilar, Carlos Allende Prieto, Stephen Bailey, Segev BenZvi, Jose Bermejo-Climent, David Brooks, Axel de la Macorra, Arjun Dey, Peter Doel, Kevin Fanning, Andreu Font-Ribera, Jaime E. Forero-Romero, Juan García-Bellido, Satya Gontcho A Gontcho, Julien Guy, ChangHoon Hahn, Klaus Honscheid, Mustapha Ishak, Stéphanie Juneau, Robert Kehoe, Theodore Kisner, Anthony Kremin, Martin Landriau, Dustin A. Lang, James Lasker, Michael E. Levi, Christophe Magneville, Christopher J. Manser, Paul Martini, Aaron M. Meisner, Ramon Miquel, John Moustakas, Jeffrey A. Newman, Jundan Nie, Nathalie. Palanque-Delabrouille, Will J. Percival, Claire Poppett, Constance Rockosi, Ashley J. Ross, Graziano Rossi, Gregory Tarlé, Benjamin A. Weaver, Christophe Yèche, Rongpu Zhou
Figure caption: Survey completeness on 2022 June 14, in the dark (top) and bright (bottom) programs. Green areas are completely finished, while white areas are unfinished. Areas not included in the footprint are in gray. Regions with E(B − V) > 0.3 are outlined by the solid contours. The dotted and dashed lines show the ecliptic and Galactic planes. The survey aims to start observations near δ = 0° and build out. Notable deviations from that pattern are areas just above δ = 30°, which are driven by needing to avoid strong winds from the south, and a region 50° from the ecliptic in the bright program in the north, driven by moon avoidance.
Paper: Survey Operations for the Dark Energy Spectroscopic Instrument
Authors: Edward F. Schlafly, David Kirkby, David J. Schlegel, Adam D. Myers, Anand Raichoor, Kyle Dawson, Jessica Aguilar, Carlos Allende Prieto, Stephen Bailey, Segev BenZvi, Jose Bermejo-Climent, David Brooks, Axel de la Macorra, Arjun Dey, Peter Doel, Kevin Fanning, Andreu Font-Ribera, Jaime E. Forero-Romero, Juan García-Bellido, Satya Gontcho A Gontcho, Julien Guy, ChangHoon Hahn, Klaus Honscheid, Mustapha Ishak, Stéphanie Juneau, Robert Kehoe, Theodore Kisner, Anthony Kremin, Martin Landriau, Dustin A. Lang, James Lasker, Michael E. Levi, Christophe Magneville, Christopher J. Manser, Paul Martini, Aaron M. Meisner, Ramon Miquel, John Moustakas, Jeffrey A. Newman, Jundan Nie, Nathalie. Palanque-Delabrouille, Will J. Percival, Claire Poppett, Constance Rockosi, Ashley J. Ross, Graziano Rossi, Gregory Tarlé, Benjamin A. Weaver, Christophe Yèche, Rongpu Zhou
Figure caption: The footprint of the DESI survey resulting from the constraints of Section 3. Tiles are colored by the amount of time it would take to reach a fixed intrinsic galaxy depth, relative to observing at zenith in the absence of Galactic extinction. This is f dust f airmass, from Equations (1) and (2). Airmasses are computed using the design airmasses resulting from the optimization of Section 4.1. The Galactic plane is shown as a dotted gray line, and the gray contour shows E(B − V) = 0.3 mag. Tiles in extinguished regions and at the decl. bounds of the survey are most expensive, owing to both atmospheric and Galactic extinction.
Paper: Survey Operations for the Dark Energy Spectroscopic Instrument
Authors: Edward F. Schlafly, David Kirkby, David J. Schlegel, Adam D. Myers, Anand Raichoor, Kyle Dawson, Jessica Aguilar, Carlos Allende Prieto, Stephen Bailey, Segev BenZvi, Jose Bermejo-Climent, David Brooks, Axel de la Macorra, Arjun Dey, Peter Doel, Kevin Fanning, Andreu Font-Ribera, Jaime E. Forero-Romero, Juan García-Bellido, Satya Gontcho A Gontcho, Julien Guy, ChangHoon Hahn, Klaus Honscheid, Mustapha Ishak, Stéphanie Juneau, Robert Kehoe, Theodore Kisner, Anthony Kremin, Martin Landriau, Dustin A. Lang, James Lasker, Michael E. Levi, Christophe Magneville, Christopher J. Manser, Paul Martini, Aaron M. Meisner, Ramon Miquel, John Moustakas, Jeffrey A. Newman, Jundan Nie, Nathalie. Palanque-Delabrouille, Will J. Percival, Claire Poppett, Constance Rockosi, Ashley J. Ross, Graziano Rossi, Gregory Tarlé, Benjamin A. Weaver, Christophe Yèche, Rongpu Zhou
Figure caption: The survey speed delivered by the DESI main survey in different programs, as measured by the ETC. The survey speed describes the rate at which (S/N)2 is accumulated relative to nominal dark conditions, and it is highest when the seeing is good and the sky is clear and dark. The dark program is observed in the best conditions, while the bright and backup programs are observed in progressively worse conditions. The legend gives the mean speed μ and the fraction of survey time spent in each program f.
Paper: Survey Operations for the Dark Energy Spectroscopic Instrument
Authors: Edward F. Schlafly, David Kirkby, David J. Schlegel, Adam D. Myers, Anand Raichoor, Kyle Dawson, Jessica Aguilar, Carlos Allende Prieto, Stephen Bailey, Segev BenZvi, Jose Bermejo-Climent, David Brooks, Axel de la Macorra, Arjun Dey, Peter Doel, Kevin Fanning, Andreu Font-Ribera, Jaime E. Forero-Romero, Juan García-Bellido, Satya Gontcho A Gontcho, Julien Guy, ChangHoon Hahn, Klaus Honscheid, Mustapha Ishak, Stéphanie Juneau, Robert Kehoe, Theodore Kisner, Anthony Kremin, Martin Landriau, Dustin A. Lang, James Lasker, Michael E. Levi, Christophe Magneville, Christopher J. Manser, Paul Martini, Aaron M. Meisner, Ramon Miquel, John Moustakas, Jeffrey A. Newman, Jundan Nie, Nathalie. Palanque-Delabrouille, Will J. Percival, Claire Poppett, Constance Rockosi, Ashley J. Ross, Graziano Rossi, Gregory Tarlé, Benjamin A. Weaver, Christophe Yèche, Rongpu Zhou
Figure caption: Completed dark time tiles have a narrow distribution in EFFTIME around the goal time of 1000 s, with tiles having on average 102% of their goal effective time, with a standard deviation of 7% (blue histogram). This demonstrates that the ETC is able to accurately predict the spectroscopic effective times from the real-time transparency, seeing, and sky brightness measurements. Bright-time tiles have a much broader range of effective time fractions and tend to be observed 30% longer than necessary (orange histogram).
Paper: Survey Operations for the Dark Energy Spectroscopic Instrument
Authors: Edward F. Schlafly, David Kirkby, David J. Schlegel, Adam D. Myers, Anand Raichoor, Kyle Dawson, Jessica Aguilar, Carlos Allende Prieto, Stephen Bailey, Segev BenZvi, Jose Bermejo-Climent, David Brooks, Axel de la Macorra, Arjun Dey, Peter Doel, Kevin Fanning, Andreu Font-Ribera, Jaime E. Forero-Romero, Juan García-Bellido, Satya Gontcho A Gontcho, Julien Guy, ChangHoon Hahn, Klaus Honscheid, Mustapha Ishak, Stéphanie Juneau, Robert Kehoe, Theodore Kisner, Anthony Kremin, Martin Landriau, Dustin A. Lang, James Lasker, Michael E. Levi, Christophe Magneville, Christopher J. Manser, Paul Martini, Aaron M. Meisner, Ramon Miquel, John Moustakas, Jeffrey A. Newman, Jundan Nie, Nathalie. Palanque-Delabrouille, Will J. Percival, Claire Poppett, Constance Rockosi, Ashley J. Ross, Graziano Rossi, Gregory Tarlé, Benjamin A. Weaver, Christophe Yèche, Rongpu Zhou
Figure caption: The number of exposures that can reach any particular point of the sky, for the seven-pass dark program, if no areas are excluded (e.g., due to low Galactic latitude or low decl.). The 12 star-like regions with slightly lower coverage correspond to the points of the underlying icosahedral tiling of Hardin et al. (2000).
Paper: Survey Operations for the Dark Energy Spectroscopic Instrument
Authors: Edward F. Schlafly, David Kirkby, David J. Schlegel, Adam D. Myers, Anand Raichoor, Kyle Dawson, Jessica Aguilar, Carlos Allende Prieto, Stephen Bailey, Segev BenZvi, Jose Bermejo-Climent, David Brooks, Axel de la Macorra, Arjun Dey, Peter Doel, Kevin Fanning, Andreu Font-Ribera, Jaime E. Forero-Romero, Juan García-Bellido, Satya Gontcho A Gontcho, Julien Guy, ChangHoon Hahn, Klaus Honscheid, Mustapha Ishak, Stéphanie Juneau, Robert Kehoe, Theodore Kisner, Anthony Kremin, Martin Landriau, Dustin A. Lang, James Lasker, Michael E. Levi, Christophe Magneville, Christopher J. Manser, Paul Martini, Aaron M. Meisner, Ramon Miquel, John Moustakas, Jeffrey A. Newman, Jundan Nie, Nathalie. Palanque-Delabrouille, Will J. Percival, Claire Poppett, Constance Rockosi, Ashley J. Ross, Graziano Rossi, Gregory Tarlé, Benjamin A. Weaver, Christophe Yèche, Rongpu Zhou
Figure caption: The fraction of the sky that is covered by a given number of tiles in the seven-pass dark tiling and the four-pass bright tiling. On average, a given part of the sky is covered by 5.2 dark tiles and 3.2 bright tiles.
Paper: CCD UBV and Gaia DR3 Analyses of the Open Clusters King 6 and NGC 1605
Authors: Sevinc Gokmen, Zeki Eker, Talar Yontan, Selçuk Bilir, Tansel Ak, Serap Ak, Timothy Banks, Ata Sarajedini
Figure caption: The RDPs of the King 6 (a) and NGC 1605 (b) OCs. The fitted black curve in each diagram is the King (1962) profile, whereas the horizontal gray band represents the background stellar density. The red-shaded domain shows the 1σ King fit uncertainty.
Paper: CCD UBV and Gaia DR3 Analyses of the Open Clusters King 6 and NGC 1605
Authors: Sevinc Gokmen, Zeki Eker, Talar Yontan, Selçuk Bilir, Tansel Ak, Serap Ak, Timothy Banks, Ata Sarajedini
Figure caption: Stellar counts of King 6 (a), (b) and NGC 1605 (c), (d) for per magnitude bin in the V and G bands. The vertical gray dashed lines show the adopted faint limiting apparent magnitudes in the V and G bands. The black lines represent the star counts in V magnitude, whereas the red dashed lines are counts in Gaia DR3 data for the same cluster regions.
Paper: CCD UBV and Gaia DR3 Analyses of the Open Clusters King 6 and NGC 1605
Authors: Sevinc Gokmen, Zeki Eker, Talar Yontan, Selçuk Bilir, Tansel Ak, Serap Ak, Timothy Banks, Ata Sarajedini
Figure caption: Distribution of cluster membership probabilities for the stars in the direction of King 6 (a) and NGC 1605 (b). The white shaded bars are the counts of stars which have been detected in the cluster regions. The cyan-colored shaded bars represent the number of stars that lie within the main-sequence band and the cluster limiting radius ﹩{r}_{\mathrm{lim}}^{\mathrm{obs}}﹩.
Paper: CCD UBV and Gaia DR3 Analyses of the Open Clusters King 6 and NGC 1605
Authors: Sevinc Gokmen, Zeki Eker, Talar Yontan, Selçuk Bilir, Tansel Ak, Serap Ak, Timothy Banks, Ata Sarajedini
Figure caption: Gaia DR3 astrometry-based VPDs of King 6 (a) and NGC 1605 (b). The membership probabilities of the stars are represented with the color scale shown on the right side. The zoomed-in boxes in panels (a) and (b) indicate the region of concentration for each cluster in the diagrams. The intersection of the dashed blue lines indicates the mean proper-motion values.
Paper: CCD UBV and Gaia DR3 Analyses of the Open Clusters King 6 and NGC 1605
Authors: Sevinc Gokmen, Zeki Eker, Talar Yontan, Selçuk Bilir, Tansel Ak, Serap Ak, Timothy Banks, Ata Sarajedini
Figure caption: CMDs of King 6 (a), (b) and NGC 1605 (c), (d) based on UBV (a), (c) and Gaia DR3 (b), (d) data. The blue lines represent the ZAMS (Sung et al. 2013) including main-sequence broadening. The membership probabilities of stars are shown with different colors. These member stars lie within ﹩{r}_{\mathrm{lim}}^{\mathrm{obs}}=10^{\prime} ﹩ of the cluster centers obtained for both clusters. The stars with low membership probabilities are plotted as gray dots.
Paper: CCD UBV and Gaia DR3 Analyses of the Open Clusters King 6 and NGC 1605
Authors: Sevinc Gokmen, Zeki Eker, Talar Yontan, Selçuk Bilir, Tansel Ak, Serap Ak, Timothy Banks, Ata Sarajedini
Figure caption:  V-band identification maps for King 6 (left panel) and NGC 1605 (right panel). The field of view of the charts is ﹩21\buildrel{\,\prime}\over{.} 5\times 21\buildrel{\,\prime}\over{.} 5﹩. North is up and east is leftward.
Paper: The Panchromatic Hubble Andromeda Treasury. XX. The Disk of M31 is Thick
Authors: Julianne J. Dalcanton, Eric F. Bell, Yumi Choi, Andrew E. Dolphin, Morgan Fouesneau, Léo Girardi, David W. Hogg, Anil C. Seth, Benjamin F. Williams
Figure caption: Maps of the apparent fraction of reddened stars for models of inclined, thickened disks where the dust is assumed to be confined to the midplane with negligible thickness compared to the stars (i.e., h  z  > > h dust). The apparent inclinations of the model disks increase from left to right (i = 15°, 30°, 45°, 60°, and 75°), and the disk thickness increases from bottom to top (h  z /h  r  = 0.05, 0.1, 0.15, and 0.2). As expected, the fraction of reddened stars is always 50% along the major axis, but deviates strongly perpendicularly, with the largest deviations seen for higher inclinations and intrinsically thicker disks. Contours indicate deviations of ±5%, ±10%, ±20%, and ±30% relative to 50%, with thicker contours indicating larger deviations.
Paper: The Panchromatic Hubble Andromeda Treasury. XX. The Disk of M31 is Thick
Authors: Julianne J. Dalcanton, Eric F. Bell, Yumi Choi, Andrew E. Dolphin, Morgan Fouesneau, Léo Girardi, David W. Hogg, Anil C. Seth, Benjamin F. Williams
Figure caption: Extremes of the fraction of reddened stars f red, using the same high-quality measurements plotted in Figure 7. The minimum values of f red (blue histogram) are calculated in regions roughly along the minor axis (θ > 110°), and the maximum values (plotted as 1 − f red; red histogram) are calculated at θ < 27°, due to lack of data along the minor axis for the highly reddened side of the disk. These maximum values are taken from much closer to the major axis, and so are not expected to have reached their asymptotal values, unlike for the minimum values of f red; this limitation is manifested as the tail to larger values of 1 − f red in the red histogram. In spite of the poorer sampling of regions with high f red, the values of f red on the obscured, near side of the disk are in good agreement with expectations from the well-sampled far side, given that the mean f red(θ > 110°) ≈ 1 − f red(θ < 27°), after culling the obvious tails at f red > 0.27 and 1 − f red > 0.32.
Paper: The Panchromatic Hubble Andromeda Treasury. XX. The Disk of M31 is Thick
Authors: Julianne J. Dalcanton, Eric F. Bell, Yumi Choi, Andrew E. Dolphin, Morgan Fouesneau, Léo Girardi, David W. Hogg, Anil C. Seth, Benjamin F. Williams
Figure caption: Map of the fraction of reddened stars f red, restricted to high-extinction (A  V  > 1.25 mag) regions with well-measured values of f red (Δf red < 0.06). There is a clear gradient in the fraction of reddened stars from the far side to the near side of the disk (i.e., left to right). The majority of the PHAT survey area, which was initially targeted to avoid M31's dust lanes, has fewer than ∼25% of its old stellar population behind the dusty ISM. The center of M31 is in the lower right, at R.A. ≈ 10.68 and decl. ≈ 41.27.
Paper: The Panchromatic Hubble Andromeda Treasury. XX. The Disk of M31 is Thick
Authors: Julianne J. Dalcanton, Eric F. Bell, Yumi Choi, Andrew E. Dolphin, Morgan Fouesneau, Léo Girardi, David W. Hogg, Anil C. Seth, Benjamin F. Williams
Figure caption: Maximum reddening fraction f red for model inclined, thickened disks, measured along the minor axis at the surface brightness corresponding to r = 3h  r  for a face-on disk. The heavy solid lines indicate the value of f red in steps of 0.1 (i.e., f red = 0.6, 0.7, etc.). The light lines indicate f red = 0.55, 0.65, etc. For thicker disks and higher inclinations, the maximum observed value of f red deviates most strongly from the naive value of f red = 0.5. The minimum value of f red at each point is one minus the plotted value.
Paper: The Panchromatic Hubble Andromeda Treasury. XX. The Disk of M31 is Thick
Authors: Julianne J. Dalcanton, Eric F. Bell, Yumi Choi, Andrew E. Dolphin, Morgan Fouesneau, Léo Girardi, David W. Hogg, Anil C. Seth, Benjamin F. Williams
Figure caption: Comparison between a Herschel Photodetector Array Camera and Spectrometer 100 μm image of emission from M31's dust (left; from Fritz et al. 2012), and an optical B-band image from the Digitized Sky Survey (right). The Herschel image shows that M31's dust content is similar on either side of the major axis. However, the stellar extinction from the dust is far more apparent on the northern (upper) half of the galaxy, leading to prominent dust lanes in the optical image. The PHAT survey footprint roughly covers the upper left quadrant of the image, extending further out in radius beyond the prominent 10 kpc ring seen in the Herschel image.
Paper: The Panchromatic Hubble Andromeda Treasury. XX. The Disk of M31 is Thick
Authors: Julianne J. Dalcanton, Eric F. Bell, Yumi Choi, Andrew E. Dolphin, Morgan Fouesneau, Léo Girardi, David W. Hogg, Anil C. Seth, Benjamin F. Williams
Figure caption: Maps of the apparent surface density for models of inclined, thickened disks, normalized to have a central surface density of unity when viewed face-on. The apparent inclinations of the model disks increase from left to right (i = 15°, 30°, 45°, 60°, and 75°), and the disk thickness increases from bottom to top (h  z /h  r  = 0.05, 0.1, 0.15, and 0.2). The white ellipse is drawn at a constant apparent surface density, equal to that seen at r = h  r  for a face-on disk. At large inclination, this isodensity contour moves to larger effective radii, due to the increased path length through the disk.
Paper: The Panchromatic Hubble Andromeda Treasury. XX. The Disk of M31 is Thick
Authors: Julianne J. Dalcanton, Eric F. Bell, Yumi Choi, Andrew E. Dolphin, Morgan Fouesneau, Léo Girardi, David W. Hogg, Anil C. Seth, Benjamin F. Williams
Figure caption: Axial ratio of model inclined, thickened disks, measured at the surface brightness corresponding to r = 1.5h  r  for a face-on disk. The heavy solid lines indicate the value of b/a in steps of 0.1 (i.e., b/a = 0.1, 0.2, etc.). The light lines indicate b/a = 0.05, 0.15, etc. For thicker disks and higher inclinations, the apparent axial ratio departs significantly from the naive expectation for an inclined, infinitely thin disk.
Paper: The Panchromatic Hubble Andromeda Treasury. XX. The Disk of M31 is Thick
Authors: Julianne J. Dalcanton, Eric F. Bell, Yumi Choi, Andrew E. Dolphin, Morgan Fouesneau, Léo Girardi, David W. Hogg, Anil C. Seth, Benjamin F. Williams
Figure caption: Representative comparison between the observed NIR stellar photometry of the RGB in a single analysis pixel (blue stars), to the expected model of the unreddened RGB (left) and to the best-fit model where a fraction f red of the RGB stars are allowed to be behind a layer of dust with a log-normal distribution of extinction characterized by a median A  V  (right). This region, drawn from the northern half of the major axis, requires a large fraction of the stars to be reddened, consistent with the visual presence of dust lanes in Figure 5. The F160W magnitude has been transformed to a reddening-free quantity, such that dust extinction and reddening move stars only to the right (Dalcanton et al. 2015).