adsabs/AstroCLIMB huggingface dataset:
Paper: A Multi-epoch, Multiwavelength Study of the Classical FUor V1515 Cyg Approaching Quiescence
Authors: Zs. M. Szabó, Á. Kóspál, P. Ábrahám, S. Park, M. Siwak, J. D. Green, A. Pál, J. A. Acosta-Pulido, J.-E. Lee, M. Ibrahimov, K. Grankin, B. Kovács, Zs. Bora, A. Bódi, B. Cseh, G. Csörnyei, Marek Dróżdż, O. Hanyecz, B. Ignácz, Cs. Kalup, R. Könyves-Tóth, M. Krezinger, L. Kriskovics, Waldemar Ogłoza, A. Ordasi, K. Sárneczky, B. Seli, R. Szakáts, Á. Sódor, A. Szing, K. Vida, J. Vinkó
Figure caption: Atomic absorption lines of Fe I 6141, Ca I 6439, Li I 6707, and Fe I 7511 Å.
Paper: A Multi-epoch, Multiwavelength Study of the Classical FUor V1515 Cyg Approaching Quiescence
Authors: Zs. M. Szabó, Á. Kóspál, P. Ábrahám, S. Park, M. Siwak, J. D. Green, A. Pál, J. A. Acosta-Pulido, J.-E. Lee, M. Ibrahimov, K. Grankin, B. Kovács, Zs. Bora, A. Bódi, B. Cseh, G. Csörnyei, Marek Dróżdż, O. Hanyecz, B. Ignácz, Cs. Kalup, R. Könyves-Tóth, M. Krezinger, L. Kriskovics, Waldemar Ogłoza, A. Ordasi, K. Sárneczky, B. Seli, R. Szakáts, Á. Sódor, A. Szing, K. Vida, J. Vinkó
Figure caption: P Cygni profiles of Hβ 4861, Hα 6562, Ca II 8542, and Ca II 8662 Å.
Paper: A Hidden Population of Massive Black Holes in Simulated Dwarf Galaxies
Authors: Ray S. Sharma, Alyson M. Brooks, Michael Tremmel, Jillian Bellovary, Angelo Ricarte, Thomas R. Quinn
Figure caption: Fraction of galaxies hosting an MBH within 10 kpc of the galaxy center, as a function of host stellar mass (left) and host halo mass (right), binned by redshift. Error bars indicate 95% binomial uncertainties. We mark observational constraints of the occupation fraction from dynamical MBH estimates (Nguyen et al. 2019; blue circles) and X-ray observations of optically selected AGN (Desroches et al. 2009; Greene 2012; green squares). We mark occupation fractions ruled out by X-ray-selected AGN (Miller et al. 2015; gray shaded). We include constraints of the occupation fraction vs. halo mass from analytic models (Buchner et al. 2019; blue dashed). At z = 2, all halos above M star > 2 × 1010 M ⊙, M 200 > 2 × 1011 M ⊙ host an MBH within 10 kpc of the center. By z = 0.05, these thresholds shift to M star > 3 × 1010 M ⊙, M 200 > 3 × 1011 M ⊙.
Paper: A Hidden Population of Massive Black Holes in Simulated Dwarf Galaxies
Authors: Ray S. Sharma, Alyson M. Brooks, Michael Tremmel, Jillian Bellovary, Angelo Ricarte, Thomas R. Quinn
Figure caption: Local z = 0.05 scaling relations colored by instantaneous Eddington fraction. Galaxies that fall below the contamination threshold, ﹩{L}_{{\rm{X}}}^{\mathrm{AGN}}\lt 2{L}_{{\rm{X}}}^{\mathrm{XRB}+\mathrm{Gas}}﹩, are marked in gray. We include X-ray-detected AGN from Birchall et al. (2020; blue crosses) and Mezcua et al. (2018; green plus signs) between 108 M ⊙ < M star < 109.5 M ⊙. Uncontaminated ROMULUS25 dwarfs are in agreement with the observed ﹩{L}_{{\rm{X}}}^{\mathrm{AGN}}-{M}_{\mathrm{star}}﹩ relation (left), ﹩{L}_{{\rm{X}}}^{\mathrm{AGN}}-\mathrm{SFR}﹩ relation (middle), and SFR−M star relation for local dwarf AGN. Contaminated galaxies do not follow observed ﹩{L}_{{\rm{X}}}^{\mathrm{AGN}}-{M}_{\mathrm{star}}﹩ or ﹩{L}_{{\rm{X}}}^{\mathrm{AGN}}-\mathrm{SFR}﹩ relations, suggesting a breakdown for undetected MBHs in dwarf galaxies.
Paper: A Hidden Population of Massive Black Holes in Simulated Dwarf Galaxies
Authors: Ray S. Sharma, Alyson M. Brooks, Michael Tremmel, Jillian Bellovary, Angelo Ricarte, Thomas R. Quinn
Figure caption: Fraction of all galaxies containing an active MBH vs. stellar mass, in bins of redshift. Activity is defined by three X-ray luminosity thresholds, ﹩\mathrm{log}{L}_{{\rm{X}}}^{\mathrm{AGN}}\gt [39,40.5,41.5]﹩. The MBH occupation fraction (black dashed) sets upper limits on the active fraction. Error bars mark 95% binomial uncertainties. Active fractions peak at z = 2 and decrease with time, at all stellar masses below M star < 1011 M ⊙. Massive galaxies exhibit consistently higher active fractions than low-mass galaxies at all times. At z = 0.05, 4% of dwarfs emit above ﹩{L}_{{\rm{X}}}^{\mathrm{AGN}}\gt {10}^{40.5}﹩ erg s−1, a factor of a few higher than found in X-ray observations from Birchall et al. (2020; circles, squares) and Mezcua et al. (2018; pentagons).
Paper: A 30 kpc Spatially Extended Clumpy and Asymmetric Galactic Outflow at z ∼ 1.7
Authors: Ahmed Shaban, Rongmon Bordoloi, John Chisholm, Soniya Sharma, Keren Sharon, Jane R. Rigby, Michael G. Gladders, Matthew B. Bayliss, L. Felipe Barrientos, Sebastian Lopez, Nicolas Tejos, Cédric Ledoux, Michael K. Florian
Figure caption: RCSGA 032727–132609 is a strong gravitationally lensed galaxy at z ≈ 1.703. Left columns: MUSE white-light images. Right columns: HST F390W, F606W, and F814W composite images. Top rows: main arc of the galaxy. Three multiple images are marked with dashed yellow rectangles. The white letters and arrows show the multiply imaged distinct star-forming regions in the image plane. Bottom rows: the counter arc of the galaxy, which shows a less magnified and distorted image of the galaxy. The yellow circles in the left panels represent the maximum seeing during the MUSE observation.
Paper: A Hidden Population of Massive Black Holes in Simulated Dwarf Galaxies
Authors: Ray S. Sharma, Alyson M. Brooks, Michael Tremmel, Jillian Bellovary, Angelo Ricarte, Thomas R. Quinn
Figure caption: The ﹩{M}_{\mathrm{BH}}^{\mathrm{acc}}-{M}_{\mathrm{star}}﹩ relation for galaxies up to M star < 1011 M ⊙ at z = 0.05. We distinguish between the brightest MBHs within 2 kpc (top) and the brightest MBHs outside of 2 kpc (bottom). Left: relation with cuts on X-ray luminosity and no cuts on contamination fraction. Colors are as in Figure 5. Right: relation with cuts on contamination fraction and no cuts on AGN luminosity. Colors are as in Figure 6. Central MBHs follow observed relations from Schramm & Silverman (2013; dashed) and Kormendy & Ho (2013; solid), while off-center MBHs exhibit higher scatter and encompass many more undermassive MBHs. Setting common detection thresholds and common contamination fractions misses many MBHs in low-mass galaxies, as well as the most undermassive MBHs at all stellar masses. Nearly all off-center MBHs are undermassive, have low luminosity, and are highly contaminated.
Paper: A 30 kpc Spatially Extended Clumpy and Asymmetric Galactic Outflow at z ∼ 1.7
Authors: Ahmed Shaban, Rongmon Bordoloi, John Chisholm, Soniya Sharma, Keren Sharon, Jane R. Rigby, Michael G. Gladders, Matthew B. Bayliss, L. Felipe Barrientos, Sebastian Lopez, Nicolas Tejos, Cédric Ledoux, Michael K. Florian
Figure caption: Mean 1D spectrum of the main arc containing the Mg II doublet. The solid black line shows the flux, and the solid cyan line shows the error in the flux. Left: the faint blue regions represent the selected wavelength window around the Mg II emission lines. The faint red regions represent the selected wavelength window for the corresponding continuum region. Right: the selection of the wavelength windows for the primary and secondary emission peaks of the Mg II 2803 emission line. The faint blue and faint red regions represent the emission and continuum windows for the primary peak, respectively. The faint green and faint yellow regions represent the emission and continuum windows for the secondary peak, respectively.
Paper: A Hidden Population of Massive Black Holes in Simulated Dwarf Galaxies
Authors: Ray S. Sharma, Alyson M. Brooks, Michael Tremmel, Jillian Bellovary, Angelo Ricarte, Thomas R. Quinn
Figure caption: The spatial number density of the brightest MBHs within 10 kpc of the halo center vs. redshift. Shown are all MBHs (purple), MBHs in dwarf galaxies with ﹩{L}_{{\rm{X}}}^{\mathrm{AGN}}\gt {10}^{39}﹩ erg s−1 and ﹩{L}_{{\rm{X}}}^{\mathrm{AGN}}\gt 2{L}_{{\rm{X}}}^{\mathrm{XRB}+\mathrm{Gas}}﹩ (solid magenta), BHs in dwarf galaxies with ﹩{L}_{{\rm{X}}}^{\mathrm{AGN}}\lt {10}^{39}﹩ erg s−1 and/or ﹩{L}_{{\rm{X}}}^{\mathrm{AGN}}\lt 2{L}_{{\rm{X}}}^{\mathrm{XRB}+\mathrm{Gas}}﹩ (dotted magenta), and all MBHs with hard ﹩\left(2-10\right)﹩ keV luminosities L X,hard > 1042 erg s−1 and ﹩{L}_{{\rm{X}}}^{\mathrm{AGN}}\gt 2{L}_{{\rm{X}}}^{\mathrm{XRB}+\mathrm{Gas}}﹩ (solid gold). Hidden MBHs in dwarf galaxies outnumber detectable MBHs by a factor of 3 and make up 40% of the overall number of MBHs in ROMULUS25 at z = 0.05. In ROMULUS25, the number density of AGN with L X,hard > 1042 erg s−1 is slightly higher than comparable estimates from observations (Ueda et al. 2014; Aird et al. 2015; Buchner et al. 2015; black square, pentagon, circle, respectively), and from the EAGLE cosmological simulation (Rosas-Guevara et al. 2016; black dotted).
Paper: A Hidden Population of Massive Black Holes in Simulated Dwarf Galaxies
Authors: Ray S. Sharma, Alyson M. Brooks, Michael Tremmel, Jillian Bellovary, Angelo Ricarte, Thomas R. Quinn
Figure caption: Active fractions vs. stellar mass for the typical two-mode accretion model (solid thick); for a single-mode accretion model with a flat radiative efficiency ϵ  r  = 0.1 (solid thin); for two-mode accretion with a flat X-ray bolometric correction, k bol,X = 25 (dotted); and for two-mode accretion with a luminosity-dependent bolometric correction derived from X-ray-selected AGN (Lusso et al. 2012; dashed). We show two luminosity thresholds ﹩{L}_{{\rm{X}}}^{\mathrm{AGN}}\gt {10}^{39}﹩ erg s−1 (purple) and ﹩{L}_{{\rm{X}}}^{\mathrm{AGN}}\gt {10}^{40.5}﹩ erg s−1 (magenta). A single-mode model yields active fractions ∼1 dex higher than observations (Birchall et al. 2020; blue points), while two-mode accretion with a factor of ∼5 higher bolometric corrections mitigates the differences above M star > 109 M ⊙.
Paper: A Hidden Population of Massive Black Holes in Simulated Dwarf Galaxies
Authors: Ray S. Sharma, Alyson M. Brooks, Michael Tremmel, Jillian Bellovary, Angelo Ricarte, Thomas R. Quinn
Figure caption: Distribution of MBH–host mass ratios at z = 0.05 among all MBHs (gray) and for MBHs with X-ray luminosities ﹩{L}_{{\rm{X}}}^{\mathrm{AGN}}\gt {10}^{39}﹩ erg s−1 (purple), ﹩{L}_{{\rm{X}}}^{\mathrm{AGN}}\gt {10}^{40.5}﹩ erg s–1 (magenta), and ﹩{L}_{{\rm{X}}}^{\mathrm{AGN}}\gt {10}^{41.5}﹩ erg s−1 (gold), binned by stellar mass. Dashed lines indicate the median of each distribution. Increasing the X-ray detection limits removes most undermassive MBHs from the detected sample in all stellar mass bins. Despite missing undermassive MBHs, raising the detection threshold does not strongly change the underlying distribution of mass ratios.
Paper: A Hidden Population of Massive Black Holes in Simulated Dwarf Galaxies
Authors: Ray S. Sharma, Alyson M. Brooks, Michael Tremmel, Jillian Bellovary, Angelo Ricarte, Thomas R. Quinn
Figure caption: Distribution of MBH–host mass ratios at z = 0.05 among all MBHs (gray) and for MBHs selected with contamination thresholds ﹩{L}_{{\rm{X}}}^{\mathrm{AGN}}\gt {f}_{\mathrm{cont}}\times {L}_{{\rm{X}}}^{\mathrm{XRB}+\mathrm{Gas}}﹩ with f cont = 1 (red), f cont = 2 (orange), and f cont = 5 (blue). Dashed lines indicate the median of each distribution. Selecting AGN with fractions as low as f cont = 1 misses most undermassive MBHs. However, raising or lowering the contamination threshold does not strongly change the underlying distribution of mass ratios.
Paper: A 30 kpc Spatially Extended Clumpy and Asymmetric Galactic Outflow at z ∼ 1.7
Authors: Ahmed Shaban, Rongmon Bordoloi, John Chisholm, Soniya Sharma, Keren Sharon, Jane R. Rigby, Michael G. Gladders, Matthew B. Bayliss, L. Felipe Barrientos, Sebastian Lopez, Nicolas Tejos, Cédric Ledoux, Michael K. Florian
Figure caption: Mean 1D spectrum of the RCSGA 032727–132609 main arc centered on the Fe II* and [O II] lines. The solid black line represents the flux and the solid cyan line represents the corresponding uncertainty of the flux. The shaded boxes show the wavelength windows used to create the Fe II* emission (faint blue), [O II] emission (faint green), and local stellar continuum (faint red and faint orange) maps, respectively. The width of the stellar continuum windows is equal to the width of the Fe II* and [O II] emission wavelength windows, respectively.
Paper: The Rate and Spatial Distribution of Novae in M31 as Determined by a 20 Year Survey
Authors: Travis A. Rector, Allen W. Shafter, William A. Burris, Matthew J. Walentosky, Kendall D. Viafore, Allison L. Strom, Richard J. Cool, Nicole A. Sola, Hannah Crayton, Catherine A. Pilachowski, George H. Jacoby, Danielle L. Corbett, Michelle Rene, Denise Hernandez
Figure caption: The number of nova candidates discovered in M31 in a given calendar year spanning the past 113 years. The average annual number of candidates detected during the seven-year period from 2015 to 2021 was 36. Assuming these candidates are all bona fide novae, this number would appear to place a stringent lower limit on the nova rate in M31.
Paper: The Rate and Spatial Distribution of Novae in M31 as Determined by a 20 Year Survey
Authors: Travis A. Rector, Allen W. Shafter, William A. Burris, Matthew J. Walentosky, Kendall D. Viafore, Allison L. Strom, Richard J. Cool, Nicole A. Sola, Hannah Crayton, Catherine A. Pilachowski, George H. Jacoby, Danielle L. Corbett, Michelle Rene, Denise Hernandez
Figure caption: The results of the numerical nova rate simulation for the ﹩20^{\prime} \times 20^{\prime} ﹩ and the ﹩36^{\prime} \times 36^{\prime} ﹩ surveyed regions of surveys A and B. The most probable nova rates in the surveyed regions are ﹩{R}_{{\rm{A}}}={17.5}_{-0.4}^{+0.9}﹩ and ﹩{R}_{{\rm{B}}}={27.0}_{-3.0}^{+3.8}﹩ per year, respectively.
Paper: The Rate and Spatial Distribution of Novae in M31 as Determined by a 20 Year Survey
Authors: Travis A. Rector, Allen W. Shafter, William A. Burris, Matthew J. Walentosky, Kendall D. Viafore, Allison L. Strom, Richard J. Cool, Nicole A. Sola, Hannah Crayton, Catherine A. Pilachowski, George H. Jacoby, Danielle L. Corbett, Michelle Rene, Denise Hernandez
Figure caption: The distribution of time between epochs, in units of log10 days.
Paper: The Rate and Spatial Distribution of Novae in M31 as Determined by a 20 Year Survey
Authors: Travis A. Rector, Allen W. Shafter, William A. Burris, Matthew J. Walentosky, Kendall D. Viafore, Allison L. Strom, Richard J. Cool, Nicole A. Sola, Hannah Crayton, Catherine A. Pilachowski, George H. Jacoby, Danielle L. Corbett, Michelle Rene, Denise Hernandez
Figure caption: The peak Hα absolute magnitudes for the novae used in our Monte Carlo analysis plotted as a function of the fade rate as measured by log(t 2). There is no evidence for an Hα MMRD relation as first demonstrated by Ciardullo et al. (1987).
Paper: The Rate and Spatial Distribution of Novae in M31 as Determined by a 20 Year Survey
Authors: Travis A. Rector, Allen W. Shafter, William A. Burris, Matthew J. Walentosky, Kendall D. Viafore, Allison L. Strom, Richard J. Cool, Nicole A. Sola, Hannah Crayton, Catherine A. Pilachowski, George H. Jacoby, Danielle L. Corbett, Michelle Rene, Denise Hernandez
Figure caption: The distribution of seeing values.
Paper: The Rate and Spatial Distribution of Novae in M31 as Determined by a 20 Year Survey
Authors: Travis A. Rector, Allen W. Shafter, William A. Burris, Matthew J. Walentosky, Kendall D. Viafore, Allison L. Strom, Richard J. Cool, Nicole A. Sola, Hannah Crayton, Catherine A. Pilachowski, George H. Jacoby, Danielle L. Corbett, Michelle Rene, Denise Hernandez
Figure caption: The number of epochs per year.
Paper: The Rate and Spatial Distribution of Novae in M31 as Determined by a 20 Year Survey
Authors: Travis A. Rector, Allen W. Shafter, William A. Burris, Matthew J. Walentosky, Kendall D. Viafore, Allison L. Strom, Richard J. Cool, Nicole A. Sola, Hannah Crayton, Catherine A. Pilachowski, George H. Jacoby, Danielle L. Corbett, Michelle Rene, Denise Hernandez
Figure caption: The completeness of surveys A and B as a function of apparent Hα magnitude as determined from the artificial nova tests.
Paper: The Rate and Spatial Distribution of Novae in M31 as Determined by a 20 Year Survey
Authors: Travis A. Rector, Allen W. Shafter, William A. Burris, Matthew J. Walentosky, Kendall D. Viafore, Allison L. Strom, Richard J. Cool, Nicole A. Sola, Hannah Crayton, Catherine A. Pilachowski, George H. Jacoby, Danielle L. Corbett, Michelle Rene, Denise Hernandez
Figure caption: The spatial distribution of the 203 novae found within our ﹩20^{\prime} \times 20^{\prime} ﹩ field of survey A, superimposed on a DSS2 red image of M31.
Paper: The Internal Proper Motion Kinematics of NGC 346: Past Formation and Future Evolution
Authors: E. Sabbi, P. Zeidler, R. P. van der Marel, A. Nota, J. Anderson, J. S. Gallagher, D. J. Lennon, L. J. Smith, M. Gennaro
Figure caption: Central plot: VPD of the stars in NGC 346 expressed in kilometers per second instead of milliarcseconds per year. The error bars represent the typical standard deviation in a bin. This information was used to determine the size of the binning step. Upper histogram: velocity distribution along the X direction. The systemic velocity (marked by the dashed-dotted black line) is ﹩{v}_{{\mathrm{sys}}_{x}}=-8.44\pm 0.20﹩ km s−1. The best-fit distribution (continuous orange line) is achieved combining two Gaussians. The center of the stronger component (blue dashed line) is at v  x1 = − 2.19 ± 0.13 km s−1 from NGC 346’s systemic velocity, with a dispersion of σ  x1 = 6.48 ± 0.20 km s−1 and number of stars at the peak of  ax1 = 160.14 ± 4.72. The broader component (dashed green line) is at v  x2 = 7.80 ± 1.87 km s−1 from the systemic velocity, with dispersion σ  x2 = 18.61 ± 2.71 km s−1 and  ax2 = 38.39 ± = 4.88 stars. Side histogram: velocity distribution along the Y direction. The systemic velocity (marked by the dashed-dotted black line) is ﹩{v}_{{\mathrm{sys}}_{y}}=10.39\pm 0.33﹩ km s−1. The best-fit distribution (continuous orange line) results from the combination of three Gaussian curves. The stronger component (dashed blue curve) is redshifted from NGC 346’s systemic velocity by v  y1 = 10.16 ± 0.38 km s−1 with dispersion σ  y1 = 7.30 ± 0.33 km s−1 and a  y1 = 111.46 ± 5.24 stars at the peak. The broader component (dashed green line) is at v  y2 = − 12.47 ± 2.16 km s−1 from NGC 346’s systemic velocity, with dispersion σ  y2 = 12.27 ± 2.29 km s−1 and a  y2 = 56.78 ± 2.05 stars. The third component (dashed purple line) is fitted with a Gaussian function with center v  y3 = − 1.37 ± 0.23 km s−1 from NGC 346’s systemic velocity, with σ  y3 = 3.09 ± 0.30 km s−1 and a  y3 = 58.90 ± 2.65 stars.
Paper: The Internal Proper Motion Kinematics of NGC 346: Past Formation and Future Evolution
Authors: E. Sabbi, P. Zeidler, R. P. van der Marel, A. Nota, J. Anderson, J. S. Gallagher, D. J. Lennon, L. J. Smith, M. Gennaro
Figure caption: The m F555W − m F814W, m F814W CMD of the stars detected in the NGC 346 region, with photometric rms <0.1 in both F814W and F555W filters. Sources with positional rms <0.1 mas yr−1 in both X and Y directions and in both epochs have been highlighted as follow: RGB stars in the magnitude range 17.9 < m F814W < 20.4 and color m F555W − m F814W > 0.5 are shown in red, and UMS stars in the magnitude ranges 17.9 < m F814W < 20.9 and color m F555W − m F814W < 0.1 are shown in blue. LMS stars fainter than m F814W < 21.9 and to the left of the line connecting m F555W − m F814W = 0.7, m F814W < 21.9 to m F555W − m F814W = 1.3, m F814W < 24.0 are marked in green. PMS stars fainter than m F814W > 21.2, to the right of the line connecting m F555W − m F814W = 0.75, m F814W < 21.2 to m F555W − m F814W = 1.5, m F814W < 24.0, with photometric rms <0.2 mag in both F814W and F555W, and positional rms <0.3 mas yr−1 in both X and Y are shown in purple.
Paper: The Internal Proper Motion Kinematics of NGC 346: Past Formation and Future Evolution
Authors: E. Sabbi, P. Zeidler, R. P. van der Marel, A. Nota, J. Anderson, J. S. Gallagher, D. J. Lennon, L. J. Smith, M. Gennaro
Figure caption: Distribution of low-mass stars, as selected from the RGB and LMS VPDs. Upper-left panel: m F555W − m F814W, m F814W CMD centered on the RGB evolutionary phase. Stars in the RGB VPD that are within 0.03 mas yr−1 from the over-density peak at μ  x  = − 0.04 mas yr−1 and μ  y  = − 0.02 mas yr−1 are shown in purple, while stars more than 0.08 mas yr−1 away from the peak are in pink. Upper-middle panel: spatial distributions of the sources found within 0.03 mas yr−1 from the over-density peak in the RGB VPD superimposed on the F555W HST image. Upper-right panel: spatial distributions of the RGB stars found more than 0.08 mas yr−1 away from the over-density peak in the RGB VPD. Lower-left panel: portion of the m F555W − m F814W, m F814W CMD centered on the LMS evolutionary phase. Stars in the LMS VPD that are within 0.03 mas yr−1 from μ  x  = − 0.04 mas yr−1 and μ  y  = − 0.02 mas yr−1 are shown in dark green, while stars more than 0.08 mas yr−1 away are in light green. The spatial distributions of the two groups of stars are shown in the lower-middle panel and lower-right panel, respectively.
Paper: The Internal Proper Motion Kinematics of NGC 346: Past Formation and Future Evolution
Authors: E. Sabbi, P. Zeidler, R. P. van der Marel, A. Nota, J. Anderson, J. S. Gallagher, D. J. Lennon, L. J. Smith, M. Gennaro
Figure caption: VPDs of the PMs for the UMS stars. The left panel shows the 5.48 × 10−17 erg cm−2 Å −1 s−1 isophotal contour level superimposed on the F555W image. This contour has been used to separate the sources likely associated with the NGC 346–N66 complex from the stars belonging to the young SMC field. The central panel shows a PM VPD of the young SMC field, and the right panel shows a VPD of the PMs for the NGC346 stars.
Paper: The Internal Proper Motion Kinematics of NGC 346: Past Formation and Future Evolution
Authors: E. Sabbi, P. Zeidler, R. P. van der Marel, A. Nota, J. Anderson, J. S. Gallagher, D. J. Lennon, L. J. Smith, M. Gennaro
Figure caption: PM VPDs measured in the F814W filter for three evolutionary phases, selected using the CMD shown in Figure 3. RGB stars are shown in the left pabel. LMS stars are in the central panel and UMS stars are in the right panel. For each population, the median error in the μ  x  and μ  y  directions is shown in the upper-right corner.
Paper: The Internal Proper Motion Kinematics of NGC 346: Past Formation and Future Evolution
Authors: E. Sabbi, P. Zeidler, R. P. van der Marel, A. Nota, J. Anderson, J. S. Gallagher, D. J. Lennon, L. J. Smith, M. Gennaro
Figure caption: 1D PM rms in milliarcseconds per year as a function of magnitude. The F555W filter is to the left and F814W to the right. The sources with positional errors <1 mas and photometric errors <0.1 mag are marked in orange. Sources with a photometric rms <0.2 mag in both filters and and with a positional rms in F814W <3 mas in both epochs are in blue.
Paper: The Internal Proper Motion Kinematics of NGC 346: Past Formation and Future Evolution
Authors: E. Sabbi, P. Zeidler, R. P. van der Marel, A. Nota, J. Anderson, J. S. Gallagher, D. J. Lennon, L. J. Smith, M. Gennaro
Figure caption: 1D position rms in milliarcsecond as a function of magnitude. The two upper panels show the results for the first epoch, while the two lower panels show the results for the second epoch. The F555W filter is to the left and F814W to the right. In both filters and epochs, we marked all the sources with positional errors <1 mas and photometric errors <0.1 mag in orange. Sources with photometric rms <0.2 mag in both filters and with positional rms in F814W <3 mas in both epochs are in blue.
Paper: The Internal Proper Motion Kinematics of NGC 346: Past Formation and Future Evolution
Authors: E. Sabbi, P. Zeidler, R. P. van der Marel, A. Nota, J. Anderson, J. S. Gallagher, D. J. Lennon, L. J. Smith, M. Gennaro
Figure caption: Left panel: mosaic footprint of the area mapped by the programs GO-10248 and GO-13680 superimposed on the DSS image. Right panel: HST color-composite image obtained combining the exposures taken by the program GO-10248. F555W is in blue and F814W in red. The positions of NGC 346 and BS90 are highlighted for convenience. North is left, east is down.