adsabs/AstroCLIMB huggingface dataset:
Paper: A Novel Survey for Young Substellar Objects with the W-band Filter. V. IC 348 and Barnard 5 in the Perseus Cloud
Authors: Bhavana Lalchand, Wen-Ping Chen, Beth A. Biller, Loïc Albert, Katelyn Allers, Sophie Dubber, Zhoujian Zhang, Michael C. Liu, Jessy Jose, Belinda Damian, Tanvi Sharma, Mickaël Bonnefoy, Yumiko Oasa
Figure caption:  J vs. J − H color–magnitude diagram for (a) IC 348 and (b) B5. The gray points represent all the CFHT WIRCam sources in the corresponding region, whereas the confirmed brown dwarfs for IC 348 (in red) and for B5 (in green) are marked. Isochrones from the AMES-Cond and AMES-DUSTY models (Allard et al. 2001) are overlapped, each adjusted by a distance modulus of 7.46 mag and E(B − V) = 0.71 (Trullols & Jordi 1997) for IC 348 and a distance modulus of 7.72 mag and E(B − V) = 0.5, 1.0, or 1.5 for B5, assuming R  v  = A  V /E(B − V) = 3.1 and the reddening law of A  J  = 0.277A  V , A  H  = 0.171A  V  (Cardelli et al. 1989).
Paper: A Novel Survey for Young Substellar Objects with the W-band Filter. V. IC 348 and Barnard 5 in the Perseus Cloud
Authors: Bhavana Lalchand, Wen-Ping Chen, Beth A. Biller, Loïc Albert, Katelyn Allers, Sophie Dubber, Zhoujian Zhang, Michael C. Liu, Jessy Jose, Belinda Damian, Tanvi Sharma, Mickaël Bonnefoy, Yumiko Oasa
Figure caption: Gaia EDR3 30′ field toward IC 348. (a) Proper-motion scatter plot (gray points), with two distinct groups marked with a red circle (Group A) and a blue circle (Group B), each with a radius of 2 mas yr−1. (b) Parallax distribution of the stars in panel (a), with Group A shown in red and Group B in blue. Stars belonging neither in Group A nor in Group B, i.e., field stars, are represented in the gray histogram. (c) Sky positions of the stars in panel (a) using the same color scheme as in panel (b), that is, red for proper-motion Group A, blue for proper-motion Group B, and gray for stars in neither group. Additionally, the black symbols represent the three confirmed substellar objects and one contaminant.
Paper: A Novel Survey for Young Substellar Objects with the W-band Filter. V. IC 348 and Barnard 5 in the Perseus Cloud
Authors: Bhavana Lalchand, Wen-Ping Chen, Beth A. Biller, Loïc Albert, Katelyn Allers, Sophie Dubber, Zhoujian Zhang, Michael C. Liu, Jessy Jose, Belinda Damian, Tanvi Sharma, Mickaël Bonnefoy, Yumiko Oasa
Figure caption: Same as Figure 11, but for Barnard 5. (a) In the proper-motion vector plot (gray points) the red symbols mark known YSOs, and the orange circle shows a radius of 2 mas yr−1 to encompass the possible range of proper motion. (b) The parallax distribution of the YSOs (in red) and of the stars within the orange circle in panel (a) but excluding the YSOs (in orange). Both the red and orange histograms use the ordinate scale on the left. All other stars outside the orange circle in panel (a) are shown as the black histogram and use the ordinate scale on the right. (c) The sky position of the three kinds of stars as in panel (b), with the same color scheme. Additionally, the blue symbols represent brown dwarf candidates, and the green symbols represent confirmed brown dwarf and the contaminants.
Paper: A Novel Survey for Young Substellar Objects with the W-band Filter. V. IC 348 and Barnard 5 in the Perseus Cloud
Authors: Bhavana Lalchand, Wen-Ping Chen, Beth A. Biller, Loïc Albert, Katelyn Allers, Sophie Dubber, Zhoujian Zhang, Michael C. Liu, Jessy Jose, Belinda Damian, Tanvi Sharma, Mickaël Bonnefoy, Yumiko Oasa
Figure caption: H-R diagram for IC 348 (red) and B5 (green) brown dwarfs overlapped with the isochrones (solid lines; 0.5–10 Myr) and evolutionary tracks (dashed lines; 0.05–0.3 M ⊙) from Baraffe et al. (2015), from where the mass and age are inferred.
Paper: A Novel Survey for Young Substellar Objects with the W-band Filter. V. IC 348 and Barnard 5 in the Perseus Cloud
Authors: Bhavana Lalchand, Wen-Ping Chen, Beth A. Biller, Loïc Albert, Katelyn Allers, Sophie Dubber, Zhoujian Zhang, Michael C. Liu, Jessy Jose, Belinda Damian, Tanvi Sharma, Mickaël Bonnefoy, Yumiko Oasa
Figure caption: Proper motion and parallax distribution of the selected regions in the Perseus complex. Each red square marks the sky position of a region, with an arrow illustrating the relative proper motion (not to scale with the coordinate axes). The number next to the square denotes the average of the parallax values (given in mas).
Paper: A Novel Survey for Young Substellar Objects with the W-band Filter. V. IC 348 and Barnard 5 in the Perseus Cloud
Authors: Bhavana Lalchand, Wen-Ping Chen, Beth A. Biller, Loïc Albert, Katelyn Allers, Sophie Dubber, Zhoujian Zhang, Michael C. Liu, Jessy Jose, Belinda Damian, Tanvi Sharma, Mickaël Bonnefoy, Yumiko Oasa
Figure caption: Same as Figure 11, but for the three star-forming regions of the Perseus molecular cloud.
Paper: Evaluating the V-band Photometric Metallicity with Fundamental Mode RR Lyrae in the Kepler Field
Authors: Chow-Choong Ngeow
Figure caption: Left panel: comparison of the instrumental (g instr − r instr) colors (in red open circles) and the calibrated (g PS1−r PS1) colors (in black filled triangles), using Equation (6), for the same RR Lyrae as presented in Figure 1. Right panel: composite of the normalized (g−r) color curve based on 27 RR Lyrae (excluding KIC 3864443, 4484128, and 7198959; due to larger scatters seen on their color curves); the red curve represents the best-fit template color curve (see the text for details).
Paper: Evaluating the V-band Photometric Metallicity with Fundamental Mode RR Lyrae in the Kepler Field
Authors: Chow-Choong Ngeow
Figure caption: An example of the plots of magStd vs. meanPSF in the g and r bands, shown in the left and right panels, respectively, for KIC 12155928. The black points are the rejected data points after the initial fitting with a third-degree polynomial function. The polynomial function was applied again to fit the remaining data points (in various colors) in the second step of the two-step fitting procedure, and displayed as the red curves. Only the data points below the red curves were selected as reference stars. All data points were extracted from the Pan-STARRS1 DR1 photometric catalogs.
Paper: Evaluating the V-band Photometric Metallicity with Fundamental Mode RR Lyrae in the Kepler Field
Authors: Chow-Choong Ngeow
Figure caption: Comparisons of the predicted gVr-band photometric [Fe/H], using Equations (9), (10), and (11) to the [Fe/H]spec for all of the 30 ab-type RR Lyrae listed in Table 2. The solid lines are the 1:1 relations, and the dashed lines represent the expected rms given in Equations (9), (10), and (11).
Paper: New Insights into the Structure of Open Clusters in the Gaia Era
Authors: Jing Zhong, 靖 钟, Li Chen, 力 陈, Yueyue Jiang, 悦悦 蒋, Songmei Qin, 松梅 秦, Jinliang Hou, 金良 侯
Figure caption: Correlation relation with r  t  and r  e  as a function of r  c  and r  h . It is clear that all correlations can be approximated with a linear relation, which suggests a correlation between the internal and external components of the cluster. The blue dashed–dotted lines are used to show the relation of y = x. In particular, we use blue dots and lines to show the radius correlation relation of clusters in sample C. The steeper slope in sample C indicates that these clusters may be affected by other dynamical processes (e.g., tidal stripping), compared with the clusters in sample H.
Paper: New Insights into the Structure of Open Clusters in the Gaia Era
Authors: Jing Zhong, 靖 钟, Li Chen, 力 陈, Yueyue Jiang, 悦悦 蒋, Songmei Qin, 松梅 秦, Jinliang Hou, 金良 侯
Figure caption: Comparison of R 50 in CG20 and r  h  in this work. As this work contains more member stars in the outer halo region, the r  h  presents a more extended distribution and is systematically larger than R 50 in CG20.
Paper: New Insights into the Structure of Open Clusters in the Gaia Era
Authors: Jing Zhong, 靖 钟, Li Chen, 力 陈, Yueyue Jiang, 悦悦 蒋, Songmei Qin, 松梅 秦, Jinliang Hou, 金良 侯
Figure caption: Left panel: radii distribution of star clusters in different age bins. Green, red, and blue colors are represent radii of r  h , r  t , r  e , respectively. Right panel: ratio of r  t /r  h  (red dots) and r  e /r  h  (blue dots) as a function of the star cluster ages. It is noted that the two panels only show the statistical relationship between the ages and radii of different star clusters but cannot be regarded as the evolution track of the single star cluster.
Paper: New Insights into the Structure of Open Clusters in the Gaia Era
Authors: Jing Zhong, 靖 钟, Li Chen, 力 陈, Yueyue Jiang, 悦悦 蒋, Songmei Qin, 松梅 秦, Jinliang Hou, 金良 侯
Figure caption: Comparison of r  c  and r  t  between K13 and this work. Left panels: histogram distributions of r  c  and r  t  radius in K13 (blue color) and this work (red color). Right panels: comparison diagrams of r  c  and r  t  radius between K13 (x-axis) and this work (y-axis). The blue dashed–dotted lines were used to show the relation of y = x. It is noted that, for most of the clusters, the r  c  in our catalog are systematically greater than in K13.
Paper: New Insights into the Structure of Open Clusters in the Gaia Era
Authors: Jing Zhong, 靖 钟, Li Chen, 力 陈, Yueyue Jiang, 悦悦 蒋, Songmei Qin, 松梅 秦, Jinliang Hou, 金良 侯
Figure caption: Relationship between the cluster boundary r 2 in K13 and the boundary of two components in our catalog. We use blue dashed–dotted lines to show the relation of y = x. Obviously, because of the existence of outer halo members, r  e  shows a larger size and can be regarded as the actual boundary of the open clusters.
Paper: A Tendency Toward Alignment in Single-star Warm-Jupiter Systems
Authors: Malena Rice, Songhu Wang, Xian-Yu Wang, Guđmundur Stefánsson, Howard Isaacson, Andrew W. Howard, Sarah E. Logsdon, Heidi Schweiker, Fei Dai, Casey Brinkman, Steven Giacalone, Rae Holcomb
Figure caption: Distribution of measured ∣λ∣ values for hot and warm Jupiters as a function of the orbital separation a/R *. Measurements in systems below the Kraft break are shown as circular markers, while those above the Kraft break are displayed as triangular markers. The new measurement of TOI-1478 b from this work is shown in yellow, and the two previous SOLES measurements are shown in peach. Saturn-mass planets are shown in gray for reference; we note that WASP-148 b falls into this category, while K2-140 b and TOI-1478 b are more massive warm Jupiters.
Paper: A Tendency Toward Alignment in Single-star Warm-Jupiter Systems
Authors: Malena Rice, Songhu Wang, Xian-Yu Wang, Guđmundur Stefánsson, Howard Isaacson, Andrew W. Howard, Sarah E. Logsdon, Heidi Schweiker, Fei Dai, Casey Brinkman, Steven Giacalone, Rae Holcomb
Figure caption: Best-fitting models for the Rossiter–McLaughlin observations obtained in this work. Left: best fit to the WIYN/NEID observations taken from the TOI-1478 b transit on UT 2022 February 5. Center: best fit to the Keck/HIRES observations taken from the TOI-1478 b transit on UT 2022 February 15. Right: joint fit incorporating both data sets.
Paper: A Tendency Toward Alignment in Single-star Warm-Jupiter Systems
Authors: Malena Rice, Songhu Wang, Xian-Yu Wang, Guđmundur Stefánsson, Howard Isaacson, Andrew W. Howard, Sarah E. Logsdon, Heidi Schweiker, Fei Dai, Casey Brinkman, Steven Giacalone, Rae Holcomb
Figure caption: Distribution of sky-projected spin–orbit angles ∣λ∣ observed for hot Jupiters (HJs), warm Jupiters (WJs), and Saturns. Unlike the hot Jupiters and Saturns, the warm Jupiters are confined to low values ∣λ∣ ≤ 20° irrespective of their host-star effective temperature.
Paper: The Infrared Medium-deep Survey. IX. Discovery of Two New z ∼ 6 Quasars and Space Density Down to M 1450 ∼ −23.5 mag
Authors: Yongjung Kim, Myungshin Im, Yiseul Jeon, Minjin Kim, Linhua Jiang, Suhyun Shin, Changsu Choi, Minhee Hyun, Hyunsung D. Jun, Dohyeong Kim, Duho Kim, Jae-Woo Kim, Ji Hoon Kim, Bumhyun Lee, Seong-Kook Lee, Juan Molina, Soojong Pak, Won-Kee Park, Yoon Chan Taak, Yongmin Yoon
Figure caption: Color–color diagram of point sources in our survey field (gray contours). The gray circles denote the 25 color-selected candidates with errors, while the arrow indicates the lower limit in color. The seven AICc-selected candidates with w  q  > 0.99 are filled with orange. The rejected candidates after the photometric cross-match with the HSC data are marked by teal crosses. The identified quasars and nonquasars are highlighted by the red open circles and crosses, respectively. The newly discovered quasars are shown as the larger symbols. The blue and purple diamonds with solid lines are the representative quasar models for ﹩{i}_{1}^{{\prime} }﹩ and ﹩{i}_{2}^{{\prime} }﹩ magnitudes, respectively, from z = 5.5 to 7.0 with a step of Δz = 0.1 with M 1450 = −24 mag, α  P  = −1.6, and logEW = 1.542. The color distributions of the whole quasar models are shown as the underneath hexagon bins in the same colors. The late-type star model is shown as the squares, color-coded by the temperature (T eff = 3000–1000 K from blue to red colors).
Paper: The Infrared Medium-deep Survey. IX. Discovery of Two New z ∼ 6 Quasars and Space Density Down to M 1450 ∼ −23.5 mag
Authors: Yongjung Kim, Myungshin Im, Yiseul Jeon, Minjin Kim, Linhua Jiang, Suhyun Shin, Changsu Choi, Minhee Hyun, Hyunsung D. Jun, Dohyeong Kim, Duho Kim, Jae-Woo Kim, Ji Hoon Kim, Bumhyun Lee, Seong-Kook Lee, Juan Molina, Soojong Pak, Won-Kee Park, Yoon Chan Taak, Yongmin Yoon
Figure caption: P200 optical spectra of four quasar candidates, after binning with resolutions of R = 956 (instrumental setup; left) and 300 (right). The blue lines represent the flux uncertainties in the 1σ level. The red lines on the spectra of J140001+554619 and J143055+531520 are their best-fit high-redshift quasar models, of which emission-line locations are marked as the red vertical ticks (Lyβ λ1025, Lyα λ1216, N V λ1240, O I λ1304, and C II λ1335 from left to right). The purple squares show the ﹩z^{\prime} ﹩-band fluxes with its bandwidth. The bottom panels show the normalized skylines. Note that the y-axis of the 2D spectra is given in units of arcsec.
Paper: The Infrared Medium-deep Survey. IX. Discovery of Two New z ∼ 6 Quasars and Space Density Down to M 1450 ∼ −23.5 mag
Authors: Yongjung Kim, Myungshin Im, Yiseul Jeon, Minjin Kim, Linhua Jiang, Suhyun Shin, Changsu Choi, Minhee Hyun, Hyunsung D. Jun, Dohyeong Kim, Duho Kim, Jae-Woo Kim, Ji Hoon Kim, Bumhyun Lee, Seong-Kook Lee, Juan Molina, Soojong Pak, Won-Kee Park, Yoon Chan Taak, Yongmin Yoon
Figure caption: Left: color distributions of the high-redshift quasar models across various redshifts (gray contours). The overplotted orange contour is for the case of ﹩{i}_{2}^{{\prime} }﹩-band magnitudes. The red and blue circles represent the spec-identified quasars from IMS and CFHQS, respectively, while the arrows indicate the lower limit of colors. Right: color distributions of the late-type star model as a function of T eff (gray squares). The overplotted orange open squares are for the case of ﹩{i}_{2}^{{\prime} }﹩-band magnitudes. The red and blue circles represent the observed late-type stars in the PS1 and CFHTLS photometric systems, respectively (see details in Section 3.3.2).
Paper: The Infrared Medium-deep Survey. IX. Discovery of Two New z ∼ 6 Quasars and Space Density Down to M 1450 ∼ −23.5 mag
Authors: Yongjung Kim, Myungshin Im, Yiseul Jeon, Minjin Kim, Linhua Jiang, Suhyun Shin, Changsu Choi, Minhee Hyun, Hyunsung D. Jun, Dohyeong Kim, Duho Kim, Jae-Woo Kim, Ji Hoon Kim, Bumhyun Lee, Seong-Kook Lee, Juan Molina, Soojong Pak, Won-Kee Park, Yoon Chan Taak, Yongmin Yoon
Figure caption: Color–color diagram of the 14 HSC-overlapped candidates (filled circles), similar to Figure 3. The blue, purple, and yellow colors represent the combinations of ﹩{i}_{1}^{{\prime} }﹩–﹩z^{\prime} ﹩–J, ﹩{i}_{2}^{{\prime} }﹩–﹩z^{\prime} ﹩–J, and ﹩{i}_{\mathrm{HSC}}^{{\prime} }﹩–﹩{z}_{\mathrm{HSC}}^{{\prime} }﹩–J, respectively. The diamonds with lines are the representative high-redshift quasar models, while the late-type star models are shown as squares with the given colors regardless of the temperature. The gray lines indicate that the connected circles are the same candidates. The spec-identified quasars are highlighted by red circles with their IDs.
Paper: The Infrared Medium-deep Survey. IX. Discovery of Two New z ∼ 6 Quasars and Space Density Down to M 1450 ∼ −23.5 mag
Authors: Yongjung Kim, Myungshin Im, Yiseul Jeon, Minjin Kim, Linhua Jiang, Suhyun Shin, Changsu Choi, Minhee Hyun, Hyunsung D. Jun, Dohyeong Kim, Duho Kim, Jae-Woo Kim, Ji Hoon Kim, Bumhyun Lee, Seong-Kook Lee, Juan Molina, Soojong Pak, Won-Kee Park, Yoon Chan Taak, Yongmin Yoon
Figure caption: Histogram of the 5σ limiting magnitudes for a point-source detection of the four survey fields. Different colors represent the magnitudes in different bands, as marked in the top panel.
Paper: The Infrared Medium-deep Survey. IX. Discovery of Two New z ∼ 6 Quasars and Space Density Down to M 1450 ∼ −23.5 mag
Authors: Yongjung Kim, Myungshin Im, Yiseul Jeon, Minjin Kim, Linhua Jiang, Suhyun Shin, Changsu Choi, Minhee Hyun, Hyunsung D. Jun, Dohyeong Kim, Duho Kim, Jae-Woo Kim, Ji Hoon Kim, Bumhyun Lee, Seong-Kook Lee, Juan Molina, Soojong Pak, Won-Kee Park, Yoon Chan Taak, Yongmin Yoon
Figure caption: Point-source detection completeness of our ﹩z^{\prime} ﹩-band images in the four survey fields. The red and blue lines are the results of including our detection criteria and detection+point-source selection criteria, respectively. The orange lines are the completeness function by Hudelot et al. (2012) that used more lenient detection criteria. The translucent lines denote the completeness of each CFHTLS tile, while the median values are highlighted by the thick solid lines.
Paper: The Infrared Medium-deep Survey. IX. Discovery of Two New z ∼ 6 Quasars and Space Density Down to M 1450 ∼ −23.5 mag
Authors: Yongjung Kim, Myungshin Im, Yiseul Jeon, Minjin Kim, Linhua Jiang, Suhyun Shin, Changsu Choi, Minhee Hyun, Hyunsung D. Jun, Dohyeong Kim, Duho Kim, Jae-Woo Kim, Ji Hoon Kim, Bumhyun Lee, Seong-Kook Lee, Juan Molina, Soojong Pak, Won-Kee Park, Yoon Chan Taak, Yongmin Yoon
Figure caption:                       ﹩{S}_{z^{\prime} }﹩ distribution of sources in the four survey fields (gray contours). The red circles denote the median ﹩{S}_{z^{\prime} }﹩ value of the artificial stars, with the 1σ (red) and 2σ (gray) levels. The dashed lines represent our point-source selection criterion of ﹩-0.006\lt {S}_{z^{\prime} }\lt 0.006﹩.
Paper: The Infrared Medium-deep Survey. IX. Discovery of Two New z ∼ 6 Quasars and Space Density Down to M 1450 ∼ −23.5 mag
Authors: Yongjung Kim, Myungshin Im, Yiseul Jeon, Minjin Kim, Linhua Jiang, Suhyun Shin, Changsu Choi, Minhee Hyun, Hyunsung D. Jun, Dohyeong Kim, Duho Kim, Jae-Woo Kim, Ji Hoon Kim, Bumhyun Lee, Seong-Kook Lee, Juan Molina, Soojong Pak, Won-Kee Park, Yoon Chan Taak, Yongmin Yoon
Figure caption: SED-fitting results for the color-selected candidates. The black circles and downward-pointing triangles are the photometric data points and their upper limits, respectively. The blue and orange lines are the best-fit high-redshift quasar and late-type star models, respectively, while the open squares in the same colors represent fluxes in each band. The key best-fit parameters of each candidate are marked in each panel. The AICc-selected candidates with w  q  > 0.99 are highlighted with star symbols.
Paper: The Infrared Medium-deep Survey. IX. Discovery of Two New z ∼ 6 Quasars and Space Density Down to M 1450 ∼ −23.5 mag
Authors: Yongjung Kim, Myungshin Im, Yiseul Jeon, Minjin Kim, Linhua Jiang, Suhyun Shin, Changsu Choi, Minhee Hyun, Hyunsung D. Jun, Dohyeong Kim, Duho Kim, Jae-Woo Kim, Ji Hoon Kim, Bumhyun Lee, Seong-Kook Lee, Juan Molina, Soojong Pak, Won-Kee Park, Yoon Chan Taak, Yongmin Yoon
Figure caption: GMOS optical spectra of two quasar candidates, dissatisfying the AICc criterion. The symbols are the same as in Figure 7.
Paper: A Novel Survey for Young Substellar Objects with the W-band Filter. V. IC 348 and Barnard 5 in the Perseus Cloud
Authors: Bhavana Lalchand, Wen-Ping Chen, Beth A. Biller, Loïc Albert, Katelyn Allers, Sophie Dubber, Zhoujian Zhang, Michael C. Liu, Jessy Jose, Belinda Damian, Tanvi Sharma, Mickaël Bonnefoy, Yumiko Oasa
Figure caption: The Q index vs. H magnitude in IC 348. Of the total 1943 sources (in gray), those likely to exhibit flux suppression due to water absorption, i.e., with Q + σ  Q  ≤ − 0.6, are marked in black (163 targets) with error bars. Those selected for spectroscopic follow up are represented in red. The orange dashed line of H = 13.5 mag indicates the nominal photometric saturation limit, whereas the one with Q = −0.6 denotes the substellar boundary for young objects. Note that the targets selected for spectroscopic follow up satisfy the water absorption and cool temperature criteria, i.e., (W1–W2) > 0.10 and (z PS1 − J CFHT) ≤ 2.
Paper: A Novel Survey for Young Substellar Objects with the W-band Filter. V. IC 348 and Barnard 5 in the Perseus Cloud
Authors: Bhavana Lalchand, Wen-Ping Chen, Beth A. Biller, Loïc Albert, Katelyn Allers, Sophie Dubber, Zhoujian Zhang, Michael C. Liu, Jessy Jose, Belinda Damian, Tanvi Sharma, Mickaël Bonnefoy, Yumiko Oasa
Figure caption: The Q index vs. H as in Figure 4 but for Barnard 5 (here with 2089 sources in gray). The black symbols mark those satisfying criteria of Q ≤ − (0.6 + σ  Q ) and H > 13.5 mag (23 targets). The red symbols mark candidates that have been followed up spectroscopically with IRTF/SpeX, and the blue symbols show candidates too faint to be observed with IRTF/SpeX. Note that both the red and blue symbol targets satisfy the water absorption and cool temperature criteria, i.e., (W1–W2) > 0.10 and (z PS1 − J CFHT) ≤ 2.
Paper: A Novel Survey for Young Substellar Objects with the W-band Filter. V. IC 348 and Barnard 5 in the Perseus Cloud
Authors: Bhavana Lalchand, Wen-Ping Chen, Beth A. Biller, Loïc Albert, Katelyn Allers, Sophie Dubber, Zhoujian Zhang, Michael C. Liu, Jessy Jose, Belinda Damian, Tanvi Sharma, Mickaël Bonnefoy, Yumiko Oasa
Figure caption: Spectral type vs. Q index of all known brown dwarfs in IC 348. The known brown dwarf list is taken from Muench et al. (2007), Luhman et al. (2016), and Alves de Oliveira et al. (2013). New discoveries from this work (confirmed spectroscopically), i.e., substellar objects, are shown in red with respective error bars. The orange dashed line denotes Q = −0.6, below which the Q value indicates a spectral type later than M6, corresponding to a substellar boundary for young objects.
Paper: A Novel Survey for Young Substellar Objects with the W-band Filter. V. IC 348 and Barnard 5 in the Perseus Cloud
Authors: Bhavana Lalchand, Wen-Ping Chen, Beth A. Biller, Loïc Albert, Katelyn Allers, Sophie Dubber, Zhoujian Zhang, Michael C. Liu, Jessy Jose, Belinda Damian, Tanvi Sharma, Mickaël Bonnefoy, Yumiko Oasa
Figure caption:  12CO (J = 1 − 0) FCRAO data of the Perseus molecular cloud (Ridge et al. 2006a). The black squares show the fields toward IC 348 and B5 covered by the W-band imaging survey. The red circles mark the fields of ∼30′ radius analyzed by using Gaia EDR3 data, including three other regions, Barnard 1, NGC 1333, and L1448 (see Section 4 for further details).
Paper: A Novel Survey for Young Substellar Objects with the W-band Filter. V. IC 348 and Barnard 5 in the Perseus Cloud
Authors: Bhavana Lalchand, Wen-Ping Chen, Beth A. Biller, Loïc Albert, Katelyn Allers, Sophie Dubber, Zhoujian Zhang, Michael C. Liu, Jessy Jose, Belinda Damian, Tanvi Sharma, Mickaël Bonnefoy, Yumiko Oasa
Figure caption: The dereddened spectra (in black) of the three candidates in IC 348 are shown in panels (a), (b), and (c), and one in B5 is shown in panel (d), with the best-fit template (in purple) shown in each case.