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REVIEW 4 major objections 4 minor 148 references

Protoplanetary Disk Survival Time-scales: A Blind Survey of Young Clusters up to 100 Myr in the Solar Vicinity

T0 review · 4 major / 4 minor · reviewed 2026-08-06 · deepseek-v4-flash

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Pith's one-line read A blind survey of 32 clusters (1–100 Myr) within 500 pc establishes wavelength-dependent disk dissipation: 1.6 ± 0.1 Myr at 1.6–4.6 microns versus 4.4 ± 0.3 Myr at 12 microns, with 120 disk candidates surviving past 10 Myr.

desk verdict A genuinely useful larger and older cluster sample confirming the wavelength-dependent disk decay, but the W4 fractions and old-disk population are detection-conditioned and need completeness work before the long timescales are quoted. read the letter →

arxiv 2507.01619 v1 pith:TLWKIR6R submitted 2025-07-02 astro-ph.SR

Gregory Mathews Ben , Jessy Jose , Jesús Hernández This is my paper
classification astro-ph.SR
keywords protoplanetarydisksdiskdispersaltimescalesyoungstarclustersinfraredexcessWISEmid-infraredphotometryGaiaclustermembershiplow-massstarsmassaccretionrates
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The reading

This paper sets out to measure how long protoplanetary disks survive by surveying 32 young clusters within 500 parsecs, spanning ages 1 to 100 million years. Using Gaia-based membership lists and infrared photometry from 1.6 to 22 $\mu$m, it finds that the disk fraction declines with cluster age at every wavelength, but on different clocks: a characteristic decay time of $\tau_{\rm short} = 1.6 \pm 0.1$ Myr for the inner disk (1.6–4.6 $\mu$m) versus $\tau_{\rm W3} = 4.4 \pm 0.3$ Myr at 12 $\mu$m. The longer clock matters because the 12 and 22 $\mu$m bands trace the outer disk, so the paper directly quantifies inside-out clearing. It also reports 120 disk candidates older than 10 Myr — 25 of them older than 30 Myr, mostly full disks around low-mass stars — and a drop in the median mass of disk-hosting stars from 0.62 to 0.27 $M_\odot$ across the 40 Myr boundary. The result extends disk lifetimes into a regime where planet formation around low-mass stars has much more time than the standard few-million-year picture allows.

What carries the argument

The argument runs on a wavelength ladder of disk detection plus an exponential decay fit. Disks are identified separately in three regimes: JHK color–color diagrams for the innermost dust; the standard Class II criteria applied to the H, K, W1, W2 bands (1.6–4.6 $\mu$m); and, for the W3 and W4 bands, a $5\sigma$ excess index $\chi = (F_{\rm obs} - F_{\rm model})/\sigma_{\rm obs}$ combined with color cuts ($J-W3 \ge 3$ mag and $K-W4 \ge 3.55$ mag) calibrated on independently known disk-bearing stars in IC 348. Each regime probes a different disk radius, with W3 corresponding to about 0.03–5 AU and W4 to 0.3–60 AU. The characteristic timescales come from fitting $f(t) = A e^{-t/\tau}$ with $A = 100$ to the cluster disk fractions, and complementary linear fits in the log(disk fraction)–log(age) plane yield the decay slopes. Because per-cluster W4 detections are sparse, an age-binned analysis pools sources across clusters to recover the statistics behind the long-wavelength fractions.

What would settle it

A mid-infrared survey reaching roughly three magnitudes deeper than the all-sky catalogues used here, over the same clusters, would settle the selection question: if the previously missed non-excess stars greatly outnumber the excess sources, the high W4 disk fractions at 6–8 Myr (92% and 86%) and the 120 old disk candidates are detection artifacts, whereas if a substantial excess population survives the deeper census, the long-lived disks are real. Optical spectroscopy of the 25 disk candidates older than 30 Myr would provide a second test, separating true low-mass stars with actively accreting disks from background giants that only mimic mid-infrared excess.

Watch

Extended reading notes

Core claim

On its own terms, the paper establishes that protoplanetary disk dissipation is wavelength-dependent in a way that maps onto disk structure: the disk fraction decays on an exponential timescale of $\tau_{\rm short} = 1.6 \pm 0.1$ Myr in the 1.6–4.6 $\mu$m bands and $\tau_{\rm W3} = 4.4 \pm 0.3$ Myr at 12 $\mu$m, with logarithmic decay slopes steepening from $-0.53$ in the W4 band to $-1.17$ in the short bands. Reading wavelength as disk radius (W3 traces roughly 0.03–5 AU, W4 roughly 0.3–60 AU), this is a quantitative confirmation of inside-out clearing: the inner disk vanishes within about 10–20 Myr while outer material lingers. The survey further finds 12 and 22 $\mu$m excesses beyond 20 Myr, with disk fractions of roughly 5–10% persisting to about 50 Myr and a population of 120 disk candidates older than 10 Myr (25 older than 30 Myr) classified mostly as full disks. The median mass of disk-hosting stars falls from 0.62 $M_\odot$ in the youngest bin to 0.27 $M_\odot$ above 40 Myr, and no disk host above 0.75 $M_\odot$ appears in the oldest bins — evidence, as the authors read it, that lower-mass stars dissipate their disks more slowly and keep planet-forming material longer.

Load-bearing premise

The load-bearing premise is that the stars detected at 12 and 22 microns fairly represent their whole clusters rather than being a brighter, disk-rich subset; the paper itself cautions that excess sources are preferentially detected in the long-wavelength bands and that some long-wavelength disk fractions must be taken cautiously.

Editorial extensions

If this is right

  • Inner disks, traced at 1.6–4.6 microns, are essentially gone within 10–20 Myr across all 32 clusters, confirming that the near-IR disk fraction drops to zero on the short clock.
  • The 2.7-times longer 12-micron timescale (4.4 Myr versus 1.6 Myr) directly quantifies inside-out clearing: the outer disk material probed at 12 microns survives roughly three times longer than the inner disk.
  • A population of 120 full disks older than 10 Myr, including 25 beyond 30 Myr, means primordial disk structures can persist far beyond the conventional ~10 Myr dissipation boundary, at least around low-mass stars.
  • Disk-hosting stars older than 40 Myr are all below about 0.75 solar masses, with median mass 0.27 solar masses, so the stars that keep their disks longest are the lowest-mass ones — the stars where planet formation therefore has the most time to operate.
  • The 33 transitional disk candidates across all age bins provide a target list for studying inner-disk clearing as it happens, and the single probable 92 Myr accretor is a candidate long-lived accreting disk (a 'Peter Pan' disk) for follow-up confirmation.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • If the old full disks are real, then 'Peter Pan' disks are not a rare curiosity but the high-age tail of a continuous, mass-dependent disk lifetime distribution; past surveys concentrated on clusters beyond roughly 250 parsecs would systematically miss most of this population because only the brightest disk hosts are detectable there.
  • The non-monotonic W3/W4 disk fraction — a minimum near 17 Myr, a secondary peak in the 20–30 Myr range, then decline — mirrors a similar trend in an independent 2024 study; if physical rather than a detection artifact, it points to a real process (delayed accretion, disk re-brightening, or a distinct late disk population) operating in that age window.
  • A clean test of the mass-dependence claim would be a spectroscopically confirmed census of disk hosts in the three old, nearby clusters (Melotte 22, IC 2602, Platais 8): the prediction is that every confirmed disk host there is an M-type star below about 0.75 solar masses.
  • For planet formation theory, the consequence of 0.27-solar-mass median disk hosts beyond 40 Myr is that low-mass stars offer up to an order of magnitude longer assembly time than the canonical few-million-year disk lifetime, shifting expectations for giant-planet formation and disk dissipation around M dwarfs.
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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

4 major / 4 minor

Summary. The paper presents a survey of protoplanetary disk fractions in 32 nearby clusters (ages ~1-100 Myr) selected from the Gaia-based Cantat-Gaudin et al. (2020) catalog, using 2MASS and WISE photometry to identify infrared excesses in the near- and mid-infrared. Disk fractions are measured in four wavelength regimes (JHK, HKW1W2, W3, W4) using three different excess-selection methods, and are fit with exponential decay functions and log-log linear relations. The authors report a monotonic decline of disk fraction with cluster age at all wavelengths, with characteristic timescales tau_short = 1.6 +/- 0.1 Myr (1.6-4.6 um) and tau_W3 = 4.4 +/- 0.3 Myr (12 um), which they interpret as evidence for inside-out disk clearing. They also identify 120 disk candidates in clusters older than 10 Myr (25 older than 30 Myr), a decrease in the median mass of disk-hosting stars from 0.62 to 0.27 Msun between young and old clusters, 33 transitional disk candidates, and 29 accretors with estimated mass accretion rates from LAMOST H-alpha spectroscopy.

Significance. If the long-wavelength results are secure, the paper would provide a valuable quantitative confirmation of inside-out disk clearing and would strengthen the case for a population of long-lived disks around low-mass stars, complementing work by Ribas et al. (2014, 2015), Pfalzner et al. (2022), and Luhman (2024). The survey's strengths include its uniform Gaia-based membership, the use of all-sky surveys to avoid small-field-of-view biases, the explicit acknowledgement of WISE sensitivity limitations (Sections 4.4 and 6.1), and the favorable comparison with independent disk-fraction measurements for short wavelengths. However, the central long-wavelength claims rest on W3/W4 samples whose denominators are WISE-detected sources, and the paper itself notes that distant W4 detections are biased toward excess sources; the age-binned W4 fractions in Table 2 (92% at 6 Myr, 86% at 8 Myr) are therefore detection-conditioned ratios rather than unbiased disk fractions.

major comments (4)
  1. [Section 4.6, Table 2; Section 4.4] The age-binned W4 disk fractions (92%, 86%, 44%, 50% at median ages 6, 8, 12, 25 Myr) are computed as excess sources divided by sources detected in W4, not by cluster members. Section 4.4 restricts the cluster-based W4 analysis to d <= 250 pc precisely because 'for the distant clusters (>250 pc), the detections in W4 band could be biased towards the excess sources,' but the binned analysis in Section 4.6 pools 'all good detections' from W3 and W4 without that restriction. Because W4 is shallow and diskless low-mass members are preferentially undetected, these binned fractions are detection-conditioned ratios. They cannot be used to support the W4 point in Figure 9 (bottom left), the fitted slope of -0.53 in Equation (10), or the claimed 22 um long-lived disk population.
  2. [Section 6.1, Equations (7)-(10); Table 1] The exponential fits f(t) = A exp(-t/tau) fix A = 100 and are applied to data with no clusters younger than 2.6 Myr, so tau_short = 1.6 +/- 0.1 Myr is anchored by an assumed initial fraction rather than measured from the youngest populations; the paper itself attributes the low value to the lack of very young clusters. More importantly, the W3 fit is strongly influenced by clusters RSG 7, RSG 8, and Trumpler 10 (Table 1) at 340-450 pc that show W3 fractions of 12-19% at 15-20 Myr, which Section 6.1 says 'must be taken cautiously.' Their W3-detected denominators are small (41-117 sources) and biased toward brighter excess sources. Removing, down-weighting, or correcting these clusters for completeness would substantially change tau_W3; as presented, tau_W3 = 4.4 +/- 0.3 Myr is not robust.
  3. [Section 6.2, Figure 10; Conclusions item 2] The 120 disk candidates older than 10 Myr are selected from the K-W3 versus K-W4 color-color diagram alone, after removing four sources with upper-limit photometry, but with no explicit rejection of background AGN or debris disks. At ages >10 Myr, 12 and 22 um excess can be produced by debris disks or by AGN coincident with cluster members; the paper's conclusion that these are 'full disks' preserving primordial structure (Conclusions item 2) requires either spectroscopic accretion diagnostics or longer-wavelength/sub-mm confirmation. Given the W3/W4 detection bias documented in Sections 4.4 and 6.1, the 25 sources older than 30 Myr may be preferentially drawn from the brightest excess sources and do not by themselves establish a primordial disk population at ~100 Myr.
  4. [Section 6.3, Figure 11 and Table 1] The claim that the median mass of disk-hosting stars decreases from 0.62 Msun to 0.27 Msun between young and old clusters is confounded by the distance-dependent sample selection. Table 1 shows that clusters with log(age) > 7.6 are predominantly within 200 pc, while most younger clusters lie beyond 300 pc, and Section 4.1 applies different mass-completeness cuts by distance (all masses within 250 pc, >0.4 Msun for 250-400 pc, >0.45 Msun beyond 400 pc). The apparent shift in median mass could therefore be a completeness artifact rather than a physical mass dependence. The manuscript should repeat the analysis restricted to the intersection mass range (e.g., 0.45-2.0 Msun) or to d <= 250 pc only; without such a test, the conclusion that lower-mass stars retain disks longer is not established by these data.
minor comments (4)
  1. [Table 2] The notation [660], [174], etc., in Table 2 is not defined in the table caption or the text; please add a footnote stating that the bracketed values are the number of disk candidates and the total number of sources, respectively.
  2. [Section 6.1, Equations (7)-(10)] The intercepts in Equations (7)-(10) are reported to two decimal places but are dimensionless logarithms; please state explicitly that log(DF) is in percent and log(age) is in Myr, and note that the fits exclude clusters with zero disk fraction, which may bias the slopes toward less negative values.
  3. [Section 3.1 and Figure 2] The Gaussian fitting procedure for cluster ages is described only briefly; please specify the initial guess, the binning of the age distribution, and how the standard error in the mean is propagated, since the cluster ages underpin all disk-fraction-versus-age fits.
  4. [Section 5] The uncertainty propagation from EW(H-alpha) and R-band flux to mass accretion rate is not described; please state whether the scatter in the Fang et al. (2009) relation is included in the quoted accretion-rate uncertainties.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the paper's central claims are empirical fits to observed disk fractions, not derivations from fitted inputs.

full rationale

The principal quantitative results (tau_short = 1.6 ± 0.1 Myr, tau_W3 = 4.4 ± 0.3 Myr, and the >10 Myr disk candidate counts) are obtained by fitting exponential and power-law functions to measured disk fractions, with the initial fraction A = 100 adopted from external literature (Fedele et al. 2010; Briceño et al. 2019). No equation in the paper predicts a quantity from a parameter that was fitted to that same quantity; the characteristic timescales are descriptive fits, explicitly labeled as such in Section 6.1. The citations to Damian et al. (2021) and Patra et al. (2024) for VOSA SED fitting and Gaussian age estimation are methodological and do not carry the central claim; the age estimates are additionally checked against literature values for IC 348, Collinder 69, IC 2602, Trumpler 10, and Melotte 22. The W3/W4 detection-bias caveats raised in Sections 4.4 and 6.1 concern completeness and selection effects, which may affect accuracy but do not make the analysis circular: the disk fractions are not constructed to equal their own inputs. The >10 Myr full-disk classification relies on color-color boundaries from Esplin et al. (2014), an external criterion, and the paper explicitly flags the need for spectroscopic confirmation. Therefore no circular step is exhibited.

Assumptions & free parameters 10 free parameters · 7 assumptions · 0 invented entities

No new physical entities are introduced. The ledger lists the parameters actually fit or chosen by hand (timescales, slopes, color thresholds, cuts) and the astrophysical models the analysis depends on. The central claims are empirical fits rather than first-principles derivations, so the parameter count is high but the circularity burden is low.

free parameters (10)
  • A (initial disk fraction in exponential fit) = 100 (adopted, not fitted)
    Anchors f(t) = A exp(-t/tau) at t = 0 because the sample lacks clusters younger than 2.6 Myr; changing A changes the fitted timescales. Section 6.1.
  • tau_short (exponential decay timescale, H, K, W1, W2) = 1.6 +/- 0.1 Myr
    Fit to cluster disk fractions; this is a headline result and a fitted constant rather than a derived prediction. Section 6.1.
  • tau_W3 (exponential decay timescale, W3 band) = 4.4 +/- 0.3 Myr
    Fit to W3 disk fractions; a headline fitted result. Section 6.1.
  • log-linear slope m for H, K, W1, W2 = -1.17 +/- 0.19
    Fit in the log(DF) versus log(age) plane; used to support wavelength-dependent decay. Equation 7.
  • log-linear slope m for W3 = -1.08 +/- 0.19
    Fit in the log(DF) versus log(age) plane; used to support wavelength-dependent decay. Equation 8.
  • log-linear slope m for W4 combined sample = -0.53 +/- 0.08
    Fit for combined own plus RBS2015 W4 data; used to show slower decay at 22 microns. Equation 10.
  • J-W3 color cutoff for W3 excess selection = 3 mag
    Chosen from the IC 348 distribution; directly sets which sources count as W3 disks. Section 4.4.
  • K-W4 color cutoff for W4 excess selection = 3.55 mag
    Adopted from Esplin et al. 2014; directly sets which sources count as W4 disks. Section 4.4.
  • W4 distance and detection cuts = d <= 250 pc and detection count > 10
    Applied to reduce W4 selection bias; leaves only 5 clusters and alters the W4 disk fraction baseline. Section 4.4.
  • Mass completeness thresholds = 0.4 Msun for 250 < d <= 400 pc; 0.45 Msun for d > 400 pc
    Defined from observed mass-distribution peaks; affects the denominator of disk fractions and the median-mass trend. Section 4.1.
assumptions (7)
  • domain assumption CG2020 Gaia DR2 membership lists with probability > 70% are reliable for cluster membership, distances, and extinctions.
    Section 2.1; the entire sample and disk fraction denominators inherit these memberships; contamination would bias all disk fractions.
  • domain assumption PARSEC 1.2 isochrones and BT-Settl SED models give reliable stellar ages and masses.
    Section 3; source ages and masses are derived from isochrone placement; model uncertainties and metallicity assumptions are not propagated.
  • domain assumption All clusters in the sample have solar metallicity.
    Section 4; assumed because the clusters are in the solar neighborhood; affects SED fits and derived ages and masses.
  • domain assumption A cluster age can be represented by the Gaussian mean of its member ages after 3-sigma clipping.
    Section 3.1; non-coeval star formation is acknowledged but treated as scatter around a single cluster age.
  • domain assumption Disk fraction decline is well described by f(t) = A exp(-t/tau).
    Section 6.1; this is a standard empirical model but a modeling choice, and A is fixed to 100.
  • domain assumption Color-color boundaries from Esplin et al. 2014 and Gutermuth et al. 2009 separate full, transitional, evolved, and debris disks.
    Sections 4.4 and 4.7; the old disk candidates are classified as full or transitional disks without spectroscopic confirmation.
  • domain assumption Accretion rate calibrations (Fang et al. 2009, White and Basri 2003, Gullbring et al. 1998) apply to the LAMOST sample.
    Section 5; used to convert H-alpha equivalent widths into mass accretion rates; calibration scatter is not propagated.

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Cite this review

Pith. "Pith review of Protoplanetary Disk Survival Time-scales: A Blind Survey of Young Clusters up to 100 Myr in the Solar Vicinity." pith.science (2026). https://pith.science/paper/TLWKIR6R

@misc{pith2026250701619,
  author       = {Pith},
  title        = {Pith review of: Protoplanetary Disk Survival Time-scales: A Blind Survey of Young Clusters up to 100 Myr in the Solar Vicinity},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/TLWKIR6R}},
  note         = {Machine review of arXiv:2507.01619}
}
abstract

We study the protoplanetary disk lifetimes using a large sample of young stellar objects in nearby clusters. To investigate the final phase of disk dissipation, we selected 32 clusters, located within 500 pc and aged between 1 and 100 Myr, with membership determined using Gaia data. The Age and mass information of the sources are obtained through spectral energy distribution (SED) analysis and using evolutionary models of various ages. Using the IR data from 2MASS and WISE catalogues, we employ three methods to identify disks across the different wavelength regimes (1.1- 22 $\mu$m). We find that disk fraction consistently decreases as stellar systems age, a trend observed across all wavelengths included in this study. However, there is an increase in the time scale of disk decay as wavelength increases, with characteristic timescales of $\tau_{\text{short}}$ = 1.6 $\pm$ 0.1 Myr for shorter wavelengths (1.6-4.6 $\mu$m) versus $\tau_{\text{W3}}$ = 4.4 $\pm$ 0.3 Myr for 12 $\mu$m. This supports the idea that outer disk regions evolve more slowly. Notably, we detect infrared excesses at 12 $\mu$m and 22 $\mu$m in relatively older systems ($>$10 Myr), with some disks with estimated ages up to $\sim$ 100 Myr. Among these, we identify a population of full disks that persist beyond the typical dissipation timescale. We also observe that the median mass of disk-hosting stars decreases from 0.62 $M_\odot$ to 0.27 $M_\odot$ in clusters younger and older than 40 Myr, respectively, indicating slower disk dissipation around lower-mass stars. We identify 33 transitional disk candidates using various color-color diagrams. Using LAMOST DR8 optical spectra and H-alpha equivalent widths, we identify possible accretors and estimate their mass accretion rates, finding most are younger than 10 Myr.

Figures

Figures reproduced from arXiv: 2507.01619 by the authors.

Figure 1
Figure 1. HR diagram of candidate members (black crosses) in a sample cluster Collinder 69. The red curves represent isochrones from the PARSEC models, arranged from top to bottom in increasing age: 0.5 Myr, 1 Myr, 5 Myr, 10 Myr, 20 Myr, and 100 Myr. of star formation leads to a spread in the age estimation as observed in several star-forming regions (Jose et al. 2016; Kraus et al. 2017; Panwar et al. 2017; Gupta et al. 2021;… view at source ↗
Figure 2
Figure 2. Age distribution of the candidate members in the cluster Collinder 69 obtained from SED and HR diagram analysis. A Gaussian profile is fitted to the distribution, and the mean of the Gaussian is considered as the age of the cluster (black dotted line). details). The mean of the Gaussian fit to this refined dataset repre￾sents the cluster’s final age, and the standard error in the mean is taken as the corresponding u… view at source ↗
Figure 3
Figure 3. Left Panel: Number of sources as a function of mass and distance. The color bar indicates the number of sources in each bin. Right Panel: Histograms showing the mass distributions; black indicates the sources within 250pc, green indicates sources with 250<d≤400 pc and red indicates sources with d>400 pc. The dashed lines correspond to the peak bin in each case. the 𝐴𝑉 associated with most of the clusters are < 1 mag… view at source ↗
Figures from the paper (8 more)
Figure 4
Figure 4. Figure 4: as an example. The red dashed line is the classical T Tauri star (CTTS) locus from Meyer et al.(1997). The green and blue curves indicate the loci of giant and main sequence stars, respectively, as determined by Bessell & Brett (1988). Two parallel dashed lines (blue a…
Figure 5
Figure 5. Figure 5: J vs J-W3 CMD of a sample cluster IC 348. The black filled circles and yellow crosses represent the members considered and class II sources identified in the region from H, K, W1 and W2 bands. The red filled circles and blue boxes indicate the excess sources from Guter…
Figure 6
Figure 6. Figure 6: Top left (Panel 1), Top right (Panel 2), Bottom left (Panel 3) and Bottom right (Panel 4) displays the disk fractions for all regions across (J,H,K), (H,K,W1,W2), W3 & W4 bands. The red dashed curve in panel 2 and panel 3 represents the exponential fit to the dataset a…
Figure 7
Figure 7. Figure 7: K-W3 vs K-W4 CCD for Bin 1. The grey dots represent all the sources in the bin and the different regions corresponds to different types of disks. The blue crosses indicate the transition disks. The red line indicates the boundary between full disks and transitional dis…
Figure 8
Figure 8. Figure 8: EW(H𝛼) vs Spectral Type plot. The red dashed line indicates the cut-off for accretors a certain order. The spectral feature of interest is then fitted with a Voigt profile, which isolates it from the continuum by excluding certain wavelength ranges surrounding the feat…
Figure 9
Figure 9. Figure 9: Top left (Panel 1),Top right (Panel 2) and Bottom left (Panel 3) display the disk fractions for all regions across (H,K,W1,W2), W3 & W4 bands in the logarithmic plane. The black dashed line represents the best-fit linear line. The red triangles in Panel 3 indicate the …
Figure 11
Figure 11. Figure 11: Mass distribution of sources with disk around them in various age bins. The blue box indicates the 90% mass range and the red line indicates the median mass for each bin. The whiskers indicates the entire mass range (< 2 M⊙) of disk sources. 6.3 Mass of the disk sourc…
Figure 12
Figure 12. Figure 12: Mass Accretion rate vs Stellar Mass plot. Red dots indicate the accretors in our sample. Blue dots are the accretors from Manara et al. 2023 older disk candidates, which adds to the limitations of our data set’s coverage. We have spectroscopic data for clusters betwee…

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Works this paper leans on

148 extracted references · 34 canonical work pages

  1. [1]

    write newline

    " write newline "" before.all 'output.state := FUNCTION fin.entry write newline FUNCTION new.block output.state before.all = 'skip after.block 'output.state := if FUNCTION new.sentence output.state after.block = 'skip output.state before.all = 'skip after.sentence 'output.state := if if FUNCTION not #0 #1 if FUNCTION and 'skip pop #0 if FUNCTION or pop #1...

  2. [2]

    C., Hollenbach D., Laughlin G., Gorti U., 2004, @doi [ ] 10.1086/421989 , https://ui.adsabs.harvard.edu/abs/2004ApJ...611..360A 611, 360

    Adams F. C., Hollenbach D., Laughlin G., Gorti U., 2004, @doi [ ] 10.1086/421989 , https://ui.adsabs.harvard.edu/abs/2004ApJ...611..360A 611, 360

    doi:10.1086/421989 2004

  3. [3]

    C., Proszkow E

    Adams F. C., Proszkow E. M., Fatuzzo M., Myers P. C., 2006, @doi [ ] 10.1086/500393 , https://ui.adsabs.harvard.edu/abs/2006ApJ...641..504A 641, 504

    doi:10.1086/500393 2006

  4. [4]

    M., et al., 2017, @doi [ ] 10.1051/0004-6361/201629929 , https://ui.adsabs.harvard.edu/abs/2017A&A...600A..20A 600, A20

    Alcal \'a J. M., et al., 2017, @doi [ ] 10.1051/0004-6361/201629929 , https://ui.adsabs.harvard.edu/abs/2017A&A...600A..20A 600, A20

    doi:10.1051/0004-6361/201629929 2017

  5. [5]

    S., Dullemond C

    Alexander R., Pascucci I., Andrews S., Armitage P., Cieza L., 2014, in Beuther H., Klessen R. S., Dullemond C. P., Henning T., eds, Protostars and Planets VI. pp 475--496 ( @eprint arXiv 1311.1819 ), @doi 10.2458/azu_uapress_9780816531240-ch021

    arXiv 2014

  6. [6]

    Alfonso J., Garc \' a-Varela A., Vieira K., 2024, @doi [ ] 10.1051/0004-6361/202450901 , https://ui.adsabs.harvard.edu/abs/2024A&A...689A..18A 689, A18

    work page doi:10.1051/0004-6361/202450901 2024

  7. [7]

    Allard F., Homeier D., et al., 2013, @doi [Memorie della Societa Astronomica Italiana Supplementi] 10.48550/arXiv.1302.6559 , https://ui.adsabs.harvard.edu/abs/2013MSAIS..24..128A 24, 128

    arXiv doi:10.48550/arxiv.1302.6559 2013

  8. [8]

    M., Wilner D

    Andrews S. M., Wilner D. J., Espaillat C., Hughes A. M., Dullemond C. P., McClure M. K., Qi C., Brown J. M., 2011, @doi [ ] 10.1088/0004-637X/732/1/42 , https://ui.adsabs.harvard.edu/abs/2011ApJ...732...42A 732, 42

    doi:10.1088/0004-637x/732/1/42 2011

Show all 148 references
  1. [9]

    Ansdell M., et al., 2016, @doi [ ] 10.3847/0004-637X/828/1/46 , https://ui.adsabs.harvard.edu/abs/2016ApJ...828...46A 828, 46

    2016 doi

  2. [10]

    J., 2013, Astrophysics of Planet Formation

    Armitage P. J., 2013, Astrophysics of Planet Formation

    2013

  3. [11]

    Ashraf M., Jose J., Herczeg G., Fang M., 2023, @doi [Journal of Astrophysics and Astronomy] 10.1007/s12036-023-09951-x , https://ui.adsabs.harvard.edu/abs/2023JApA...44...67A 44, 67

    2023 doi

  4. [12]

    Rodrigo, C

    Bayo, A. Rodrigo, C. Barrado y Navascu\'es, D. et al., 2008, @doi [A&A] 10.1051/0004-6361:200810395 , 492, 277

    2008 doi

  5. [13]

    Bayo A., et al., 2011, @doi [ ] 10.1051/0004-6361/201116617 , https://ui.adsabs.harvard.edu/abs/2011A&A...536A..63B 536, A63

    2011 doi

  6. [14]

    S., Brett J

    Bessell M. S., Brett J. M., 1988, @doi [ ] 10.1086/132281 , https://ui.adsabs.harvard.edu/abs/1988PASP..100.1134B 100, 1134

    1988 doi

  7. [15]

    M., Covino E., Frasca A., Getman F., Spezzi L., 2012, @doi [ ] 10.1051/0004-6361/201219680 , https://ui.adsabs.harvard.edu/abs/2012A&A...547A.104B 547, A104

    Biazzo K., Alcal \'a J. M., Covino E., Frasca A., Getman F., Spezzi L., 2012, @doi [ ] 10.1051/0004-6361/201219680 , https://ui.adsabs.harvard.edu/abs/2012A&A...547A.104B 547, A104

    2012 doi

  8. [16]

    P., 2011, @doi [ ] 10.1088/0004-637X/731/1/74 , https://ui.adsabs.harvard.edu/abs/2011ApJ...731...74B 731, 74

    Boss A. P., 2011, @doi [ ] 10.1088/0004-637X/731/1/74 , https://ui.adsabs.harvard.edu/abs/2011ApJ...731...74B 731, 74

    2011 doi

  9. [17]

    Bouvier J., Alencar S. H. P., Harries T. J., Johns-Krull C. M., Romanova M. M., 2007, in Reipurth B., Jewitt D., Keil K., eds, Protostars and Planets V. p. 479 ( @eprint arXiv astro-ph/0603498 ), @doi 10.48550/arXiv.astro-ph/0603498

    2007 doi arXiv

  10. [18]

    D., Eisner J

    Boyden R. D., Eisner J. A., 2020, @doi [ ] 10.3847/1538-4357/ab86b7 , https://ui.adsabs.harvard.edu/abs/2020ApJ...894...74B 894, 74

    2020 doi

  11. [20]

    Brice \ n o C., et al., 2019, @doi [ ] 10.3847/1538-3881/aaf79b , https://ui.adsabs.harvard.edu/abs/2019AJ....157...85B 157, 85

    2019 doi

  12. [21]

    G., et al., 2011, @doi [ ] 10.1007/s11207-010-9541-4 , https://ui.adsabs.harvard.edu/abs/2011SoPh..268..255C 268, 255

    Caffau E., Ludwig H. G., et al., 2011, @doi [ ] 10.1007/s11207-010-9541-4 , https://ui.adsabs.harvard.edu/abs/2011SoPh..268..255C 268, 255

    2011 doi

  13. [22]

    Calvet N., Gullbring E., 1998, @doi [ ] 10.1086/306527 , https://ui.adsabs.harvard.edu/abs/1998ApJ...509..802C 509, 802

    1998 doi

  14. [23]

    Calvet N., et al., 2005, @doi [ ] 10.1086/491652 , https://ui.adsabs.harvard.edu/abs/2005ApJ...630L.185C 630, L185

    2005 doi

  15. [24]

    Cantat-Gaudin T., Anders F., Castro-Ginard A., et al., 2020, @doi [ ] 10.1051/0004-6361/202038192 , https://ui.adsabs.harvard.edu/abs/2020A&A...640A...1C 640, A1

    2020 doi

  16. [25]

    M., 2001, @doi [ ] 10.1086/320383 , https://ui.adsabs.harvard.edu/abs/2001AJ....121.2851C 121, 2851

    Carpenter J. M., 2001, @doi [ ] 10.1086/320383 , https://ui.adsabs.harvard.edu/abs/2001AJ....121.2851C 121, 2851

    2001 doi

  17. [26]

    M., Mamajek E

    Carpenter J. M., Mamajek E. E., Hillenbrand L. A., Meyer M. R., 2006, @doi [ ] 10.1086/509121 , https://ui.adsabs.harvard.edu/abs/2006ApJ...651L..49C 651, L49

    2006 doi

  18. [27]

    Chabrier G., 2003, @doi [ ] 10.1086/376392 , https://ui.adsabs.harvard.edu/abs/2003PASP..115..763C 115, 763

    2003 doi

  19. [28]

    C., et al., 2016, @doi [arXiv e-prints] 10.48550/arXiv.1612.05560 , https://ui.adsabs.harvard.edu/abs/2016arXiv161205560C p

    Chambers K. C., et al., 2016, @doi [arXiv e-prints] 10.48550/arXiv.1612.05560 , https://ui.adsabs.harvard.edu/abs/2016arXiv161205560C p. arXiv:1612.05560

    2016 doi arXiv

  20. [29]

    Coleman G. A. L., Haworth T. J., 2020, @doi [ ] 10.1093/mnrasl/slaa098 , https://ui.adsabs.harvard.edu/abs/2020MNRAS.496L.111C 496, L111

    2020 doi

  21. [30]

    Coleman G. A. L., Haworth T. J., 2022, @doi [ ] 10.1093/mnras/stac1513 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.514.2315C 514, 2315

    2022 doi

  22. [31]

    Cui X.-Q., et al., 2012, @doi [Research in Astronomy and Astrophysics] 10.1088/1674-4527/12/9/003 , https://ui.adsabs.harvard.edu/abs/2012RAA....12.1197C 12, 1197

    2012 doi

  23. [32]

    E., Hillenbrand L

    Dahm S. E., Hillenbrand L. A., 2007, @doi [ ] 10.1086/512156 , https://ui.adsabs.harvard.edu/abs/2007AJ....133.2072D 133, 2072

    2007 doi

  24. [33]

    R., Moraux E., Das S

    Damian B., Jose J., Samal M. R., Moraux E., Das S. R., Patra S., 2021, @doi [ ] 10.1093/mnras/stab194 , https://ui.adsabs.harvard.edu/abs/2021MNRAS.504.2557D 504, 2557

    2021 doi

  25. [34]

    T., 2023, @doi [Journal of Astrophysics and Astronomy] 10.1007/s12036-023-09968-2 , https://ui.adsabs.harvard.edu/abs/2023JApA...44...77D 44, 77

    Damian B., Jose J., Biller B., Paul K. T., 2023, @doi [Journal of Astrophysics and Astronomy] 10.1007/s12036-023-09968-2 , https://ui.adsabs.harvard.edu/abs/2023JApA...44...77D 44, 77

    2023 doi

  26. [35]

    Damian B., et al., 2024, @doi [ ] 10.1093/mnras/stae2452 , https://ui.adsabs.harvard.edu/abs/2024MNRAS.535.1321D 535, 1321

    2024 doi

  27. [36]

    R., Jose J., Samal M

    Das S. R., Jose J., Samal M. R., Zhang S., Panwar N., 2021, @doi [ ] 10.1093/mnras/staa3222 , https://ui.adsabs.harvard.edu/abs/2021MNRAS.500.3123D 500, 3123

    2021 doi

  28. [37]

    R., Gupta S., Prakash P., Samal M., Jose J., 2023, @doi [ ] 10.3847/1538-4357/acbf54 , https://ui.adsabs.harvard.edu/abs/2023ApJ...948....7D 948, 7

    Das S. R., Gupta S., Prakash P., Samal M., Jose J., 2023, @doi [ ] 10.3847/1538-4357/acbf54 , https://ui.adsabs.harvard.edu/abs/2023ApJ...948....7D 948, 7

    2023 doi

  29. [38]

    R., Gupta S., Jose J., Samal M., Herczeg G

    Das S. R., Gupta S., Jose J., Samal M., Herczeg G. J., Guo Z., More S., Prakash P., 2025, @doi [arXiv e-prints] 10.48550/arXiv.2503.16205 , https://ui.adsabs.harvard.edu/abs/2025arXiv250316205D p. arXiv:2503.16205

    2025 doi arXiv

  30. [39]

    M., et al., 2014, in Beuther H., Klessen R

    Dunham M. M., et al., 2014, in Beuther H., Klessen R. S., Dullemond C. P., Henning T., eds, Protostars and Planets VI. pp 195--218 ( @eprint arXiv 1401.1809 ), @doi 10.2458/azu_uapress_9780816531240-ch009

    2014 arXiv

  31. [40]

    M., et al., 2015, @doi [The Astrophysical Journal Supplement Series] 10.1088/0067-0049/220/1/11 , 220, 11

    Dunham M. M., et al., 2015, @doi [The Astrophysical Journal Supplement Series] 10.1088/0067-0049/220/1/11 , 220, 11

    2015 doi

  32. [41]

    K., Samal M

    Dutta S., Mondal S., Jose J., Das R. K., Samal M. R., Ghosh S., 2015, @doi [ ] 10.1093/mnras/stv2190 , https://ui.adsabs.harvard.edu/abs/2015MNRAS.454.3597D 454, 3597

    2015 doi

  33. [42]

    Espaillat C., et al., 2012, @doi [ ] 10.1088/0004-637X/747/2/103 , https://ui.adsabs.harvard.edu/abs/2012ApJ...747..103E 747, 103

    2012 doi

  34. [43]

    L., Luhman K

    Esplin T. L., Luhman K. L., Mamajek E. E., 2014, @doi [ ] 10.1088/0004-637X/784/2/126 , https://ui.adsabs.harvard.edu/abs/2014ApJ...784..126E 784, 126

    2014 doi

  35. [44]

    L., Luhman K

    Esplin T. L., Luhman K. L., Miller E. B., Mamajek E. E., 2018, @doi [ ] 10.3847/1538-3881/aacce0 , https://ui.adsabs.harvard.edu/abs/2018AJ....156...75E 156, 75

    2018 doi

  36. [45]

    J., Bisbas T

    Facchini S., Clarke C. J., Bisbas T. G., 2016, @doi [ ] 10.1093/mnras/stw240 , https://ui.adsabs.harvard.edu/abs/2016MNRAS.457.3593F 457, 3593

    2016 doi

  37. [46]

    Fang M., van Boekel R., Wang W., Carmona A., Sicilia-Aguilar A., Henning T., 2009, @doi [ ] 10.1051/0004-6361/200912468 , https://ui.adsabs.harvard.edu/abs/2009A&A...504..461F 504, 461

    2009 doi

  38. [47]

    J., Rizzuto A., 2017, @doi [ ] 10.3847/1538-4357/aa74ca , https://ui.adsabs.harvard.edu/abs/2017ApJ...842..123F 842, 123

    Fang Q., Herczeg G. J., Rizzuto A., 2017, @doi [ ] 10.3847/1538-4357/aa74ca , https://ui.adsabs.harvard.edu/abs/2017ApJ...842..123F 842, 123

    2017 doi

  39. [48]

    E., Henning T., Jayawardhana R., Oliveira J

    Fedele D., van den Ancker M. E., Henning T., Jayawardhana R., Oliveira J. M., 2010, @doi [ ] 10.1051/0004-6361/200912810 , https://ui.adsabs.harvard.edu/abs/2010A&A...510A..72F 510, A72

    2010 doi

  40. [49]

    Fiorellino E., et al., 2021, @doi [ ] 10.1051/0004-6361/202039264 , https://ui.adsabs.harvard.edu/abs/2021A&A...650A..43F 650, A43

    2021 doi

  41. [50]

    S., Dullemond C

    Frank A., et al., 2014, in Beuther H., Klessen R. S., Dullemond C. P., Henning T., eds, Protostars and Planets VI. pp 451--474 ( @eprint arXiv 1402.3553 ), @doi 10.2458/azu_uapress_9780816531240-ch020

    2014 arXiv

  42. [51]

    M., Manara C

    Frasca A., Biazzo K., Alcal \'a J. M., Manara C. F., Stelzer B., Covino E., Antoniucci S., 2017, @doi [ ] 10.1051/0004-6361/201630108 , https://ui.adsabs.harvard.edu/abs/2017A&A...602A..33F 602, A33

    2017 doi

  43. [52]

    Gaia Collaboration et al., 2016, @doi [ ] 10.1051/0004-6361/201629272 , https://ui.adsabs.harvard.edu/abs/2016A&A...595A...1G 595, A1

    2016 doi

  44. [53]

    Garcia Lopez R., Natta A., Testi L., Habart E., 2006, @doi [ ] 10.1051/0004-6361:20065575 , https://ui.adsabs.harvard.edu/abs/2006A&A...459..837G 459, 837

    2006 doi

  45. [54]

    P., Hollenbach D., 2009, @doi [ ] 10.1088/0004-637X/705/2/1237 , https://ui.adsabs.harvard.edu/abs/2009ApJ...705.1237G 705, 1237

    Gorti U., Dullemond C. P., Hollenbach D., 2009, @doi [ ] 10.1088/0004-637X/705/2/1237 , https://ui.adsabs.harvard.edu/abs/2009ApJ...705.1237G 705, 1237

    2009 doi

  46. [55]

    L., et al., 2021, @doi [ ] 10.3847/1538-4357/abf432 , https://ui.adsabs.harvard.edu/abs/2021ApJ...913..123G 913, 123

    Grant S. L., et al., 2021, @doi [ ] 10.3847/1538-4357/abf432 , https://ui.adsabs.harvard.edu/abs/2021ApJ...913..123G 913, 123

    2021 doi

  47. [56]

    G., et al., 2021, @doi [ ] 10.1051/0004-6361/202140361 , https://ui.adsabs.harvard.edu/abs/2021A&A...650A.157G 650, A157

    Guarcello M. G., et al., 2021, @doi [ ] 10.1051/0004-6361/202140361 , https://ui.adsabs.harvard.edu/abs/2021A&A...650A.157G 650, A157

    2021 doi

  48. [57]

    Gullbring E., Hartmann L., et al., 1998, @doi [ ] 10.1086/305032 , https://ui.adsabs.harvard.edu/abs/1998ApJ...492..323G 492, 323

    1998 doi

  49. [58]

    Gupta S., et al., 2021, @doi [ ] 10.1093/mnras/stab2751 , https://ui.adsabs.harvard.edu/abs/2021MNRAS.508.3388G 508, 3388

    2021 doi

  50. [59]

    R., Guo Z., Damian B., Prakash P., Samal M

    Gupta S., Jose J., Das S. R., Guo Z., Damian B., Prakash P., Samal M. R., 2024, @doi [ ] 10.1093/mnras/stae369 , https://ui.adsabs.harvard.edu/abs/2024MNRAS.528.5633G 528, 5633

    2024 doi

  51. [60]

    A., Megeath S

    Gutermuth R. A., Megeath S. T., Myers P. C., Allen L. E., Pipher J. L., Fazio G. G., 2009, @doi [The Astrophysical Journal Supplement Series] 10.1088/0067-0049/184/1/18 , 184, 18

    2009 doi

  52. [61]

    Haerken H., Li G.-W., Li M., Duan F., Zhao Y., 2024, @doi [ ] 10.3847/1538-4357/ad04d3 , https://ui.adsabs.harvard.edu/abs/2024ApJ...960...58H 960, 58

    2024 doi

  53. [62]

    J., Lada E

    Haisch Karl E. J., Lada E. A., Lada C. J., 2001, @doi [ ] 10.1086/320685 , https://ui.adsabs.harvard.edu/abs/2001ApJ...553L.153H 553, L153

    2001 doi

  54. [63]

    M., Clarke C

    Hall S. M., Clarke C. J., Pringle J. E., 1996, @doi [ ] 10.1093/mnras/278.2.303 , https://ui.adsabs.harvard.edu/abs/1996MNRAS.278..303H 278, 303

    1996 doi

  55. [64]

    Hartmann L., Herczeg G., Calvet N., 2016, @doi [ ] 10.1146/annurev-astro-081915-023347 , https://ui.adsabs.harvard.edu/abs/2016ARA&A..54..135H 54, 135

    2016 doi

  56. [65]

    S., Dullemond C

    Helled R., et al., 2014, in Beuther H., Klessen R. S., Dullemond C. P., Henning T., eds, Protostars and Planets VI. pp 643--665 ( @eprint arXiv 1311.1142 ), @doi 10.2458/azu_uapress_9780816531240-ch028

    2014 arXiv

  57. [66]

    J., Hillenbrand L

    Herczeg G. J., Hillenbrand L. A., 2008, @doi [ ] 10.1086/586728 , https://ui.adsabs.harvard.edu/abs/2008ApJ...681..594H 681, 594

    2008 doi

  58. [67]

    J., Hillenbrand L

    Herczeg G. J., Hillenbrand L. A., 2015, @doi [The Astrophysical Journal] 10.1088/0004-637x/808/1/23 , 808, 23

    2015 doi

  59. [68]

    Hern \'a ndez J., et al., 2007, @doi [ ] 10.1086/513735 , https://ui.adsabs.harvard.edu/abs/2007ApJ...662.1067H 662, 1067

    2007 doi

  60. [69]

    Hern \'a ndez J., Calvet N., Hartmann L., Muzerolle J., Gutermuth R., Stauffer J., 2009, @doi [ ] 10.1088/0004-637X/707/1/705 , https://ui.adsabs.harvard.edu/abs/2009ApJ...707..705H 707, 705

    2009 doi

  61. [70]

    Hern \'a ndez J., et al., 2023, @doi [ ] 10.3847/1538-3881/acc467 , https://ui.adsabs.harvard.edu/abs/2023AJ....165..205H 165, 205

    2023 doi

  62. [71]

    A., 2008, @doi [Physica Scripta Volume T] 10.1088/0031-8949/2008/T130/014024 , https://ui.adsabs.harvard.edu/abs/2008PhST..130a4024H 130, 014024

    Hillenbrand L. A., 2008, @doi [Physica Scripta Volume T] 10.1088/0031-8949/2008/T130/014024 , https://ui.adsabs.harvard.edu/abs/2008PhST..130a4024H 130, 014024

    2008 doi

  63. [72]

    Hou W., et al., 2016, @doi [Research in Astronomy and Astrophysics] 10.1088/1674-4527/16/9/138 , https://ui.adsabs.harvard.edu/abs/2016RAA....16..138H 16, 138

    2016 doi

  64. [73]

    Jose J., et al., 2012, @doi [ ] 10.1111/j.1365-2966.2012.21175.x , https://ui.adsabs.harvard.edu/abs/2012MNRAS.424.2486J 424, 2486

    2012

  65. [74]

    S., Herczeg G

    Jose J., Kim J. S., Herczeg G. J., Samal M. R., Bieging J. H., Meyer M. R., Sherry W. H., 2016, @doi [ ] 10.3847/0004-637X/822/1/49 , https://ui.adsabs.harvard.edu/abs/2016ApJ...822...49J 822, 49

    2016 doi

  66. [75]

    J., Samal M

    Jose J., Herczeg G. J., Samal M. R., Fang Q., Panwar N., 2017, @doi [ ] 10.3847/1538-4357/836/1/98 , https://ui.adsabs.harvard.edu/abs/2017ApJ...836...98J 836, 98

    2017 doi

  67. [76]

    Jose J., et al., 2020, @doi [ ] 10.3847/1538-4357/ab74dd , https://ui.adsabs.harvard.edu/abs/2020ApJ...892..122J 892, 122

    2020 doi

  68. [77]

    P., Leisawitz D

    Koenig X. P., Leisawitz D. T., 2014, @doi [ ] 10.1088/0004-637X/791/2/131 , https://ui.adsabs.harvard.edu/abs/2014ApJ...791..131K 791, 131

    2014 doi

  69. [78]

    L., Ireland M

    Kraus A. L., Ireland M. J., Hillenbrand L. A., Martinache F., 2012, @doi [ ] 10.1088/0004-637X/745/1/19 , https://ui.adsabs.harvard.edu/abs/2012ApJ...745...19K 745, 19

    2012 doi

  70. [79]

    L., Herczeg G

    Kraus A. L., Herczeg G. J., Rizzuto A. C., Mann A. W., Slesnick C. L., Carpenter J. M., Hillenbrand L. A., Mamajek E. E., 2017, @doi [ ] 10.3847/1538-4357/aa62a0 , https://ui.adsabs.harvard.edu/abs/2017ApJ...838..150K 838, 150

    2017 doi

  71. [80]

    Kroupa P., 2001, @doi [ ] 10.1046/j.1365-8711.2001.04022.x , https://ui.adsabs.harvard.edu/abs/2001MNRAS.322..231K 322, 231

    2001

  72. [81]

    Kroupa P., 2002, @doi [Science] 10.1126/science.1067524 , https://ui.adsabs.harvard.edu/abs/2002Sci...295...82K 295, 82

    2002 doi

  73. [82]

    W., Schlegel D

    Lang D., Hogg D. W., Schlegel D. J., 2016, @doi [ ] 10.3847/0004-6256/151/2/36 , https://ui.adsabs.harvard.edu/abs/2016AJ....151...36L 151, 36

    2016 doi

  74. [83]

    Laos S., et al., 2022, @doi [ ] 10.3847/1538-4357/ac8156 , https://ui.adsabs.harvard.edu/abs/2022ApJ...935..111L 935, 111

    2022 doi

  75. [84]

    Lawson K., et al., 2023, @doi [The Astronomical Journal] 10.3847/1538-3881/aced08 , 166, 150

    2023 doi

  76. [85]

    L., 2022, @doi [ ] 10.3847/1538-3881/ac35e2 , https://ui.adsabs.harvard.edu/abs/2022AJ....163...24L 163, 24

    Luhman K. L., 2022, @doi [ ] 10.3847/1538-3881/ac35e2 , https://ui.adsabs.harvard.edu/abs/2022AJ....163...24L 163, 24

    2022 doi

  77. [86]

    L., 2024, @doi [ ] 10.3847/1538-3881/ad697d , https://ui.adsabs.harvard.edu/abs/2024AJ....168..159L 168, 159

    Luhman K. L., 2024, @doi [ ] 10.3847/1538-3881/ad697d , https://ui.adsabs.harvard.edu/abs/2024AJ....168..159L 168, 159

    2024 doi

  78. [87]

    L., Mamajek E

    Luhman K. L., Mamajek E. E., 2012, @doi [ ] 10.1088/0004-637X/758/1/31 , https://ui.adsabs.harvard.edu/abs/2012ApJ...758...31L 758, 31

    2012 doi

  79. [88]

    B., Heggie D

    Malmberg D., Davies M. B., Heggie D. C., 2011, @doi [ ] 10.1111/j.1365-2966.2010.17730.x , https://ui.adsabs.harvard.edu/abs/2011MNRAS.411..859M 411, 859

    2011

  80. [89]

    E., 2009, in Usuda T., Tamura M., Ishii M., eds, American Institute of Physics Conference Series Vol

    Mamajek E. E., 2009, in Usuda T., Tamura M., Ishii M., eds, American Institute of Physics Conference Series Vol. 1158, Exoplanets and Disks: Their Formation and Diversity. AIP, pp 3--10 ( @eprint arXiv 0906.5011 ), @doi 10.1063/1.3215910

    2009 arXiv

  81. [90]

    F., et al., 2016, @doi [Astronomy & amp; Astrophysics] 10.1051/0004-6361/201628549 , 591, L3

    Manara C. F., et al., 2016, @doi [Astronomy & amp; Astrophysics] 10.1051/0004-6361/201628549 , 591, L3

    2016 doi

  82. [91]

    F., Ansdell M., Rosotti G

    Manara C. F., Ansdell M., Rosotti G. P., Hughes A. M., Armitage P. J., Lodato G., Williams J. P., 2023, in Inutsuka S., Aikawa Y., Muto T., Tomida K., Tamura M., eds, Astronomical Society of the Pacific Conference Series Vol. 534, Protostars and Planets VII. p. 539 ( @eprint a...

    2023 doi arXiv

  83. [92]

    Manzo-Mart \' nez E., et al., 2020, @doi [ ] 10.3847/1538-4357/ab7ead , https://ui.adsabs.harvard.edu/abs/2020ApJ...893...56M 893, 56

    2020 doi

  84. [93]

    Masana E., Jordi C., Ribas I., 2006, @doi [ ] 10.1051/0004-6361:20054021 , https://ui.adsabs.harvard.edu/abs/2006A&A...450..735M 450, 735

    2006 doi

  85. [94]

    Mathew B., et al., 2018, @doi [The Astrophysical Journal] 10.3847/1538-4357/aab3d8 , 857, 30

    2018 doi

  86. [95]

    Mauc \'o K., et al., 2025, @doi [ ] 10.1051/0004-6361/202452386 , https://ui.adsabs.harvard.edu/abs/2025A&A...693A..87M 693, A87

    2025 doi

  87. [96]

    Mendigut \' a I., Solano E., Vioque M., Balaguer-Nu \ n ez L., Ribas A., Hu \'e lamo N., Rodrigo C., 2022, @doi [ ] 10.1051/0004-6361/202243146 , https://ui.adsabs.harvard.edu/abs/2022A&A...664A..66M 664, A66

    2022 doi

  88. [97]

    Meng H. Y. A., Rieke G. H., Su K. Y. L., G \'a sp \'a r A., 2017, @doi [ ] 10.3847/1538-4357/836/1/34 , https://ui.adsabs.harvard.edu/abs/2017ApJ...836...34M 836, 34

    2017 doi

  89. [98]

    R., Calvet N., Hillenbrand L

    Meyer M. R., Calvet N., Hillenbrand L. A., 1997, @doi [ ] 10.1086/118474 , https://ui.adsabs.harvard.edu/abs/1997AJ....114..288M 114, 288

    1997 doi

  90. [99]

    R., Backman D

    Meyer M. R., Backman D. E., Weinberger A. J., Wyatt M. C., 2007, in Reipurth B., Jewitt D., Keil K., eds, Protostars and Planets V. p. 573 ( @eprint arXiv astro-ph/0606399 ), @doi 10.48550/arXiv.astro-ph/0606399

    2007 doi arXiv

  91. [100]

    C., Kataoka A., 2023, in Inutsuka S., Aikawa Y., Muto T., Tomida K., Tamura M., eds, Astronomical Society of the Pacific Conference Series Vol

    Miotello A., Kamp I., Birnstiel T., Cleeves L. C., Kataoka A., 2023, in Inutsuka S., Aikawa Y., Muto T., Tomida K., Tamura M., eds, Astronomical Society of the Pacific Conference Series Vol. 534, Protostars and Planets VII. p. 501 ( @eprint arXiv 2203.09818 ), @doi 10.48550/ar...

    2023 doi arXiv

  92. [101]

    J., Mamajek E

    Murphy S. J., Mamajek E. E., Bell C. P. M., 2018, @doi [ ] 10.1093/mnras/sty471 , https://ui.adsabs.harvard.edu/abs/2018MNRAS.476.3290M 476, 3290

    2018 doi

  93. [102]

    Muzerolle J., Hillenbrand L., Calvet N., Briceño C., Hartmann L., 2003, @doi [The Astrophysical Journal] 10.1086/375704 , 592, 266

    2003 doi

  94. [103]

    Natta A., Testi L., Randich S., 2006, @doi [ ] 10.1051/0004-6361:20054706 , https://ui.adsabs.harvard.edu/abs/2006A&A...452..245N 452, 245

    2006 doi

  95. [104]

    S., 2023, @doi [Journal of Astrophysics and Astronomy] 10.1007/s12036-023-09965-5 , https://ui.adsabs.harvard.edu/abs/2023JApA...44...75N 44, 75

    Nidhi S., Mathew B., Shridharan B., Bhattacharyya S., Edwin D., Kartha S. S., 2023, @doi [Journal of Astrophysics and Astronomy] 10.1007/s12036-023-09965-5 , https://ui.adsabs.harvard.edu/abs/2023JApA...44...75N 44, 75

    2023 doi

  96. [105]

    H., White R

    Nisak A. H., White R. J., Yep A., Henry T. J., Paredes L., James H.-S., Jao W.-C., 2022, @doi [ ] 10.3847/1538-3881/ac63c3 , https://ui.adsabs.harvard.edu/abs/2022AJ....163..278N 163, 278

    2022 doi

  97. [106]

    T., Alam M., DeLaurentiis S., 2022, PHEW: PytHon Equivalent Widths , @doi 10.5281/zenodo.6422571

    N \'u \ n ez A., Douglas S. T., Alam M., DeLaurentiis S., 2022, PHEW: PytHon Equivalent Widths , @doi 10.5281/zenodo.6422571

    2022 doi

  98. [107]

    K., et al., 2004, @doi [The Astrophysical Journal] 10.1086/425068 , 616, 1042–1057

    Ojha D. K., et al., 2004, @doi [The Astrophysical Journal] 10.1086/425068 , 616, 1042–1057

    2004 doi

  99. [108]

    M., Garc \' a Hern \'a ndez A., Su \'a rez Yanes J

    Pamos Ortega D., Mirouh G. M., Garc \' a Hern \'a ndez A., Su \'a rez Yanes J. C., Barcel \'o Forteza S., 2023, @doi [ ] 10.1051/0004-6361/202346323 , https://ui.adsabs.harvard.edu/abs/2023A&A...675A.167P 675, A167

    2023 doi

  100. [109]

    Panwar N., et al., 2017, @doi [ ] 10.1093/mnras/stx616 , https://ui.adsabs.harvard.edu/abs/2017MNRAS.468.2684P 468, 2684

    2017 doi

  101. [110]

    R., Lahuis F., Natta A., 2009, @doi [ ] 10.1088/0004-637X/696/1/143 , https://ui.adsabs.harvard.edu/abs/2009ApJ...696..143P 696, 143

    Pascucci I., Apai D., Luhman K., Henning T., Bouwman J., Meyer M. R., Lahuis F., Natta A., 2009, @doi [ ] 10.1088/0004-637X/696/1/143 , https://ui.adsabs.harvard.edu/abs/2009ApJ...696..143P 696, 143

    2009 doi

  102. [111]

    K., 2023, in Inutsuka S., Aikawa Y., Muto T., Tomida K., Tamura M., eds, Astronomical Society of the Pacific Conference Series Vol

    Pascucci I., Cabrit S., Edwards S., Gorti U., Gressel O., Suzuki T. K., 2023, in Inutsuka S., Aikawa Y., Muto T., Tomida K., Tamura M., eds, Astronomical Society of the Pacific Conference Series Vol. 534, Protostars and Planets VII. p. 567 ( @eprint arXiv 2203.10068 ), @doi 10...

    2023 doi arXiv

  103. [112]

    J., 2024, @doi [ ] 10.3847/1538-4357/ad4996 , https://ui.adsabs.harvard.edu/abs/2024ApJ...970...88P 970, 88

    Patra S., Jose J., Evans N. J., 2024, @doi [ ] 10.3847/1538-4357/ad4996 , https://ui.adsabs.harvard.edu/abs/2024ApJ...970...88P 970, 88

    2024 doi

  104. [113]

    J., Mamajek E

    Pecaut M. J., Mamajek E. E., 2013, @doi [The Astrophysical Journal Supplement Series] 10.1088/0067-0049/208/1/9 , 208, 9

    2013 doi

  105. [114]

    Pfalzner S., Dincer F., 2024, @doi [ ] 10.3847/1538-4357/ad1bef , https://ui.adsabs.harvard.edu/abs/2024ApJ...963..122P 963, 122

    2024 doi

  106. [115]

    Pfalzner S., Steinhausen M., Menten K., 2014, @doi [ ] 10.1088/2041-8205/793/2/L34 , https://ui.adsabs.harvard.edu/abs/2014ApJ...793L..34P 793, L34

    2014 doi

  107. [116]

    Pfalzner S., Dehghani S., Michel A., 2022, @doi [ ] 10.3847/2041-8213/ac9839 , https://ui.adsabs.harvard.edu/abs/2022ApJ...939L..10P 939, L10

    2022 doi

  108. [117]

    Picogna G., Marzari F., 2014, @doi [ ] 10.1051/0004-6361/201322816 , https://ui.adsabs.harvard.edu/abs/2014A&A...564A..28P 564, A28

    2014 doi

  109. [118]

    E., Weber M

    Picogna G., Ercolano B., Owen J. E., Weber M. L., 2019, @doi [ ] 10.1093/mnras/stz1166 , https://ui.adsabs.harvard.edu/abs/2019MNRAS.487..691P 487, 691

    2019 doi

  110. [119]

    C., 2021, @doi [ ] 10.1093/mnras/stab2883 , https://ui.adsabs.harvard.edu/abs/2021MNRAS.508.3611P 508, 3611

    Picogna G., Ercolano B., Espaillat C. C., 2021, @doi [ ] 10.1093/mnras/stab2883 , https://ui.adsabs.harvard.edu/abs/2021MNRAS.508.3611P 508, 3611

    2021 doi

  111. [120]

    Ribas \'A ., Mer \' n B., et al., 2014, @doi [ ] 10.1051/0004-6361/201322597 , https://ui.adsabs.harvard.edu/abs/2014A&A...561A..54R 561, A54

    2014 doi

  112. [121]

    Ribas \'A ., Bouy H., Mer \' n B., 2015, @doi [ ] 10.1051/0004-6361/201424846 , https://ui.adsabs.harvard.edu/abs/2015A&A...576A..52R 576, A52

    2015 doi

  113. [122]

    Ribas \'A ., et al., 2023, @doi [ ] 10.1051/0004-6361/202245637 , https://ui.adsabs.harvard.edu/abs/2023A&A...673A..77R 673, A77

    2023 doi

  114. [124]

    Richert A. J. W., Getman K. V., Feigelson E. D., Kuhn M. A., Broos P. S., Povich M. S., Bate M. R., Garmire G. P., 2018b, @doi [Monthly Notices of the Royal Astronomical Society] 10.1093/mnras/sty949 , 477, 5191–5206

    doi

  115. [125]

    S., Sicilia-Aguilar A., Lawson W

    Roccatagliata V., Bouwman J., Henning T., Gennaro M., Feigelson E., Kim J. S., Sicilia-Aguilar A., Lawson W. A., 2011, @doi [ ] 10.1088/0004-637X/733/2/113 , https://ui.adsabs.harvard.edu/abs/2011ApJ...733..113R 733, 113

    2011 doi

  116. [126]

    Ru \' z-Rodr \' guez D., et al., 2018, @doi [ ] 10.1093/mnras/sty1351 , https://ui.adsabs.harvard.edu/abs/2018MNRAS.478.3674R 478, 3674

    2018 doi

  117. [127]

    R., Pandey A

    Samal M. R., Pandey A. K., Ojha D. K., Chauhan N., Jose J., Pandey B., 2012, @doi [ ] 10.1088/0004-637X/755/1/20 , https://ui.adsabs.harvard.edu/abs/2012ApJ...755...20S 755, 20

    2012 doi

  118. [128]

    Schneider G., et al., 2014, @doi [ ] 10.1088/0004-6256/148/4/59 , https://ui.adsabs.harvard.edu/abs/2014AJ....148...59S 148, 59

    2014 doi

  119. [129]

    Sicilia-Aguilar A., et al., 2006, @doi [ ] 10.1086/498085 , https://ui.adsabs.harvard.edu/abs/2006ApJ...638..897S 638, 897

    2006 doi

  120. [130]

    M., et al., 2020, @doi [The Astrophysical Journal] 10.3847/1538-4357/ab68e6 , 890, 106

    Silverberg S. M., et al., 2020, @doi [The Astrophysical Journal] 10.3847/1538-4357/ab68e6 , 890, 106

    2020 doi

  121. [131]

    F., Cutri R

    Skrutskie M. F., Cutri R. M., et al., 2006, @doi [ ] 10.1086/498708 , https://ui.adsabs.harvard.edu/abs/2006AJ....131.1163S 131, 1163

    2006 doi

  122. [132]

    R., Hillenbrand L

    Soderblom D. R., Hillenbrand L. A., Jeffries R. D., Mamajek E. E., Naylor T., 2014, in Beuther H., Klessen R. S., Dullemond C. P., Henning T., eds, Protostars and Planets VI. pp 219--241 ( @eprint arXiv 1311.7024 ), @doi 10.2458/azu_uapress_9780816531240-ch010

    2014 arXiv

  123. [133]

    G., Torres G., 2016, @doi [ ] 10.3847/2041-8205/831/1/L6 , https://ui.adsabs.harvard.edu/abs/2016ApJ...831L...6S 831, L6

    Stassun K. G., Torres G., 2016, @doi [ ] 10.3847/2041-8205/831/1/L6 , https://ui.adsabs.harvard.edu/abs/2016ApJ...831L...6S 831, L6

    2016 doi

  124. [134]

    Sugitani K., et al., 2002, @doi [ ] 10.1086/339196 , https://ui.adsabs.harvard.edu/abs/2002ApJ...565L..25S 565, L25

    2002 doi

  125. [135]

    Thanathibodee T., Calvet N., Hern \'a ndez J., Mauc \'o K., Brice \ n o C., 2022, @doi [ ] 10.3847/1538-3881/ac3ee6 , https://ui.adsabs.harvard.edu/abs/2022AJ....163...74T 163, 74

    2022 doi

  126. [136]

    J., et al., 2020, @doi [ ] 10.3847/1538-4357/ab6f64 , https://ui.adsabs.harvard.edu/abs/2020ApJ...890..130T 890, 130

    Tobin J. J., et al., 2020, @doi [ ] 10.3847/1538-4357/ab6f64 , https://ui.adsabs.harvard.edu/abs/2020ApJ...890..130T 890, 130

    2020 doi

  127. [137]

    Venuti L., et al., 2014, @doi [ ] 10.1051/0004-6361/201423776 , https://ui.adsabs.harvard.edu/abs/2014A&A...570A..82V 570, A82

    2014 doi

  128. [138]

    Villenave M., et al., 2020, @doi [ ] 10.1051/0004-6361/202038087 , https://ui.adsabs.harvard.edu/abs/2020A&A...642A.164V 642, A164

    2020 doi

  129. [139]

    Vlasblom M., De Marchi G., 2023, @doi [ ] 10.1051/0004-6361/202245248 , https://ui.adsabs.harvard.edu/abs/2023A&A...675A.204V 675, A204

    2023 doi

  130. [140]

    A., Ren B., Kalas P., Carpenter J., 2021, @doi [ ] 10.1093/mnras/stab1080 , https://ui.adsabs.harvard.edu/abs/2021MNRAS.504.3074W 504, 3074

    Walker S., Millar-Blanchaer M. A., Ren B., Kalas P., Carpenter J., 2021, @doi [ ] 10.1093/mnras/stab1080 , https://ui.adsabs.harvard.edu/abs/2021MNRAS.504.3074W 504, 3074

    2021 doi

  131. [141]

    Wang S., Chen X., 2019, @doi [ ] 10.3847/1538-4357/ab1c61 , https://ui.adsabs.harvard.edu/abs/2019ApJ...877..116W 877, 116

    2019 doi

  132. [142]

    J., Basri G., 2003, @doi [The Astrophysical Journal] 10.1086/344673 , 582, 1109

    White R. J., Basri G., 2003, @doi [The Astrophysical Journal] 10.1086/344673 , 582, 1109

    2003 doi

  133. [144]

    P., Cieza L

    Williams J. P., Cieza L. A., 2011b, @doi [ ] 10.1146/annurev-astro-081710-102548 , https://ui.adsabs.harvard.edu/abs/2011ARA&A..49...67W 49, 67

    doi

  134. [145]

    J., Clarke C

    Winter A. J., Clarke C. J., Rosotti G., Ih J., Facchini S., Haworth T. J., 2018, @doi [ ] 10.1093/mnras/sty984 , https://ui.adsabs.harvard.edu/abs/2018MNRAS.478.2700W 478, 2700

    2018 doi

  135. [146]

    L., Eisenhardt P

    Wright E. L., Eisenhardt P. R. M., et al., 2010, @doi [ ] 10.1088/0004-6256/140/6/1868 , https://ui.adsabs.harvard.edu/abs/2010AJ....140.1868W 140, 1868

    2010 doi

  136. [147]

    T., Saito M., 2014, @doi [ ] 10.1093/mnras/stu1013 , https://ui.adsabs.harvard.edu/abs/2014MNRAS.442.2543Y 442, 2543

    Yasui C., Kobayashi N., Tokunaga A. T., Saito M., 2014, @doi [ ] 10.1093/mnras/stu1013 , https://ui.adsabs.harvard.edu/abs/2014MNRAS.442.2543Y 442, 2543

    2014 doi

  137. [148]

    Yasui C., Kobayashi N., Saito M., Izumi N., Skidmore W., 2021, @doi [ ] 10.3847/1538-3881/abd331 , https://ui.adsabs.harvard.edu/abs/2021AJ....161..139Y 161, 139

    2021 doi

  138. [149]

    arXiv:1206.3569

    Zhao G., Zhao Y., Chu Y., Jing Y., Deng L., 2012, @doi [arXiv e-prints] 10.48550/arXiv.1206.3569 , https://ui.adsabs.harvard.edu/abs/2012arXiv1206.3569Z p. arXiv:1206.3569

    2012 doi arXiv

  139. [150]

    Zuckerman B., Song I., 2004, @doi [ ] 10.1146/annurev.astro.42.053102.134111 , https://ui.adsabs.harvard.edu/abs/2004ARA&A..42..685Z 42, 685

    2004

  140. [151]

    D., 2021, @doi [ ] 10.3847/1538-3881/ac0255 , https://ui.adsabs.harvard.edu/abs/2021AJ....162...28V 162, 28

    van der Marel N., Mulders G. D., 2021, @doi [ ] 10.3847/1538-3881/ac0255 , https://ui.adsabs.harvard.edu/abs/2021AJ....162...28V 162, 28

    2021 doi

Pith tools

Reviewed August 6, 2026 · model on record in the stance chip above.