# Debris disk color with the Hubble Space Telescope

Bin B Ren, Isabel Rebollido, Élodie Choquet, Wen-Han Zhou, Marshall D Perrin, Glenn Schneider, Julien Milli, Schuyler G Wolff, Christine H Chen, John H Debes, et al.

► To cite this version:

Bin B Ren, Isabel Rebollido, Élodie Choquet, Wen-Han Zhou, Marshall D Perrin, et al. Debris disk color with the Hubble Space Telescope. Astronomy and Astrophysics - A&A, 2023, 672, pp.A114. 10.1051/0004-6361/202245458. [https://arxiv.org/abs/2004.04548](https://arxiv.org/abs/2004.04548). [hal-04168633](https://HAL Id: hal-04168633)

Submitted on 21 Jul 2023

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<figure><img src="image_1.png" /></figure>

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# Debris disk color with the Hubble Space Telescope*

Bin B. Ren (任彬)<fnref n="1" />,<fnref n="2" />,<fnref n="3" /> Ⓓ, Isabel Rebollido<fnref n="4" />, Élodie Choquet<fnref n="5" /> Ⓓ, Wen-Han Zhou (周文翰)<fnref n="1" /> Ⓓ, Marshall D. Perrin<fnref n="4" /> Ⓓ, Glenn Schneider<fnref n="6" />, Julien Milli<fnref n="2" /> Ⓓ, Schuyler G. Wolff<fnref n="6" /> Ⓓ, Christine H. Chen<fnref n="4" /> Ⓓ, John H. Debes<fnref n="4" />, J. Brendan Hagan<fnref n="4" />, Dean C. Hines<fnref n="4" /> Ⓓ, Maxwell A. Millar-Blanchaer<fnref n="8" />, Laurent Pueyo<fnref n="4" />, Aki Roberge<fnref n="9" /> Ⓓ, Eugene Serabyn<fnref n="7" />, and Rémi Soumerme<fnref n="4" /> Ⓓ

Received 14 November 2022 / Accepted 8 February 2023

## ABSTRACT

**Context.** Multiwavelength scattered light imaging of debris disks may inform dust properties including typical size and mineral composition. Existing studies have investigated a small set of individual systems across a variety of imaging instruments and filters, calling for uniform comparison studies to systematically investigate dust properties.

**Aims.** We obtain the surface brightness of dust particles in debris disks by post-processing coronagraphic imaging observations, and compare the multiwavelength reflectance of dust. For a sample of resolved debris disks, we perform a systematic analysis on the reflectance properties of their birth rings.

**Methods.** We reduced the visible and near-infrared images of 23 debris disk systems hosted by A through M stars using two coronagraphs on board the *Hubble* Space Telescope: the STIS instrument observations centered at 0.58 µm, and the NICMOS instrument at 1.12 µm or 1.60 µm. For proper recovery of debris disks, we used classical reference differential imaging for STIS, and adopted non-negative matrix factorization with forward modeling for NICMOS. By dividing disk signals by stellar signals to take into account intrinsic stellar color effects, we systematically obtained and compared the reflectance of debris birth rings at ≈90° scattering angle.

**Results.** Debris birth rings typically exhibit a blue color at ≈90° scattering angle. As the stellar luminosity increases, the color tends to be more neutral. A likely L-shaped color-albedo distribution indicates a clustering of scatterer properties.

**Conclusions.** The observed color trend correlates with the expected blow-out size of dust particles. The color-albedo clustering likely suggests different populations of dust in these systems. More detailed radiative transfer models with realistic dust morphology will contribute to explaining the observed color and color-albedo distribution of debris systems.

**Key words.** stars: imaging – instrumentation: high angular resolution – Kuiper belt: general – techniques: image processing

## 1. Introduction

Debris disks are extrasolar analogs of the Asteroid Belt and the Kuiper Belt (e.g., Hughes et al. 2018). They are composed of second-generation dust, in the sense that their life time is shorter than the age of their host star (e.g., Wyatt 2008), and they are produced from and continuously replenished by collisional cascades of larger solid bodies (Dohnanyi 1969). While collisional cascades produce small dust particles, radiation pressure can surpass gravity for small dust particles and blow certain dust particles out of stellar systems (e.g., Strubbe & Chiang 2006; Krivov et al. 2006). The balance of forces for dust particles results in a blow-out size that ranges from submicron to several microns depending on both stellar properties and dust properties

(e.g., spectral type, dust composition, dust porosity; Arnold et al. 2019). Observationally, depending on the blow-out size and other dust properties in disks, there could be noticeable differences (e.g., scattering phase function: Muñoz et al. 2021).

In the birth ring of a debris disk, dust particles under collisional cascade have an expected number distribution $n(a) \propto a^{-3.5}$, where a is the particle size (e.g., Pan & Schlichting 2012). Assuming that the cross section of each particle is proportional to $a^2$, a collisional cascade can make the smaller particles dominate more surface area of a debris disk. In reality, stellar radiation pressure can drive smaller particles to higher eccentricity or even unbound orbits, resulting in blow-out sizes above which dust particles are bound. Nevertheless, the balance between radiation and gravity predicts that dust particles can be unbound only within a certain size range (e.g., Thebault & Kral 2019), and that there is no stellar radiation-driven blow-out size for certain latter-type stars (e.g., M stars: Arnold et al. 2019). Other mechanisms, including stellar winds in M stars (e.g., AU Mic: Augereau & Beust 2006, TWA 7: Olofsson et al. 2020), can also remove dust

<footnote n="1">¹ Université Côte d'Azur, Observatoire de la Côte d'Azur, CNRS, Laboratoire Lagrange, 06304 Nice, France
e-mail: bin.ren@oca.eu</footnote>

<footnote n="2">² Université Grenoble Alpes, CNRS, Institut de Planétologie et d'Astrophysique (IPAG), 38000 Grenoble, France</footnote>

<footnote n="3">³ Department of Astronomy, California Institute of Technology, MC 249-17, 1200 East California Boulevard, Pasadena, CA 91125, USA</footnote>

<footnote n="4">⁴ Space Telescope Science Institute (STScI), 3700 San Martin Drive, Baltimore, MD 21218, USA</footnote>

<footnote n="5">⁵ Aix-Marseille Univ, CNRS, CNES, LAM, Marseille, France</footnote>

<footnote n="6">⁶ Steward Observatory, The University of Arizona, Tucson, AZ 85721, USA</footnote>

<footnote n="7">⁷ Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA</footnote>

<footnote n="8">⁸ Department of Physics, University of California, Santa Barbara, CA 93106, USA</footnote>

<footnote n="9">⁹ Astrophysics Science Division, NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA</footnote>

<footnote>* Data for Figs. 2, 3, and 4 are only available at the CDS
via anonymous ftp to cdsarc.cds.unistra.fr (130.79.128.5)
or via https://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/
672/A114</footnote>
particles from stellar environments, complicating the size distri-
bution of dust in debris systems. The joint effect of these mech-
anisms could lead to observational complexity for debris disks.

Studies on the spectral energy distribution (SED) of debris
disks show that the ratio of dust temperature to blackbody tem-
perature at the disk radius decreases with increasing stellar
luminosity (e.g., Pawellek et al. 2014). Although this trend can
be explained by the hypothesis that typical dust size increases
with stellar luminosity (Pawellek et al. 2014; Pawellek & Krivov
2015), the blackbody location of disks can be offset from their
resolved locations by a factor of ~4 (e.g., scattered light imaging:
Esposito et al. 2020) since debris dust particles are inefficient
emitters at longer wavelengths. This offset makes SED modeling
a degenerate problem between dust property and disk location.
With resolved disk images in scattered light, we can break these
known degeneracies for the smallest dust in debris systems.

Using a variety of coronagraphic imaging instruments from
the ground (e.g., NaCo: Lagrange et al. 2003; Lenzen et al. 2003,
GPI: Macintosh et al. 2008, SPHERE: Beuzit et al. 2008) and
from space (e.g., ACS: Ford et al. 1998, NICMOS: Ramberg
1993, STIS: Woodgate et al. 1998), multiwavelength scattered
light imaging studies revealed dust properties for debris disks
individually, such as 49 Ceti (Choquet et al. 2017; Pawellek et
2019), AU Mic (Fitzgerald et al. 2007), Beta Pic (Golimowski
et al. 2006), HD 15115 (Kalas et al. 2007), HD 32297 (Kalas
2005; Duchêne et al. 2020), HD 35841 (Esposito et al. 2018),
HD 107146 (Ertel et al. 2011), HD 191089 (Ren et al. 2019),
HD 192758 (Choquet et al. 2018), HR 4796A (Debes et al. 2008;
Milli et al. 2015; Rodigas et al. 2015; Chen et al. 2020; Arriaga
et al. 2020), and TWA 7 (Ren et al. 2021). These multiwave-
length studies, when further augmented with the advantage of
uniform imaging exploration from identical instruments (e.g.,
GPI debris disk survey: Esposito et al. 2020), would minimize
the offsets from different instruments to enable uniform sys-
tematic studies of dust properties, and would thus bring forth
essential information on the ensemble properties of debris disks
in scattered light.

With debris disks resolved in scattered light, existing studies
have investigated their ensemble properties, especially on scat-
tering phase functions (SPFs), which depict the scattered light
intensity dependence on scattering angles. Hughes et al. (2018)
suggested that the SPF of debris disks could follow a uniform
trend; however, more recent observations with high-precision
measurements showed diverse SPF in different systems (e.g.,
Ren et al. 2019; Engler et al. 2022) or even potential SPF change
at different wavelengths (e.g., Ren et al. 2020). In addition,
SPF measurements could be impacted by instrumentation effects
including convolution, by data reduction artifacts such as overfit-
ting and self-subtraction in high-contrast total intensity imaging,
and by vertical thickness effects (e.g., Milli et al. 2017; Olofsson
et al. 2020); these complications make it necessary to study
debris disks from another complementary perspective, namely
multiband imaging (e.g., Chen et al. 2020; Arriaga et al. 2020),
to depict their collective properties.

On board the *Hubble* Space Telescope (HST), the Space Telescope Imaging Spectrograph (STIS: Woodgate et al. 1998) and Near Infrared Camera and Multi-Object Spectrometer (NICMOS: Thompson 1992) instruments can offer unparalleled stability and sensitivity in the coronagraphic imaging of circumstellar disks from visible light to near-infrared wavelengths. In comparison with protoplanetary disks that are relatively bright and easily observed from ground-based extreme-adaptive-optics-equipped systems in polarized light (e.g., Avenhaus et al. 2018; Laws et al. 2020), HST coronagraphs can offer both stable

stellar point spread function (PSF) and optimal sensitivity for faint target imaging. These advanced instruments provide the most effective method for imaging faint debris disks in total intensity (e.g., STIS: Krist et al. 2010, 2012; Schneider et al. 2018). In addition, HST operates in vacuum, which makes it more straightforward to calibrate detector readouts to physical units (e.g., Viana et al. 2009) than ground-based observations (e.g., Milli et al. 2015); it is also sensitive to the faintest materials such as debris halos that are elusive from the ground (e.g., halos: Schneider et al. 2018; Ren et al. 2019).

With the high stability, high sensitivity, and high spatial
resolution offered by HST, resolved scattered light imaging of
debris disks can directly probe the spatial and surface bright-
ness distributions for the smallest dust particles within (e.g.,
Schneider et al. 2014, 2018). When imaged at multiple wave-
lengths, the color information of the scatterers can inform dust
properties (e.g., composition, porosity: Debes et al. 2008). In
addition, resolved imaging of debris disks enabled by the appli-
cation of advanced statistical methods, especially when applied
to archival observations and recovering the hidden debris disks
(e.g., Soummer et al. 2014; Choquet et al. 2014), can allow the
study of dust properties to an unprecedented degree (e.g., albedo:
Choquet et al. 2018). Combining the advantages of multiwave-
length images offered by HST and disk recovery from advanced
methods, here we perform a uniform recovery and study of
resolved debris disks to investigate their ensemble properties.
We describe the observation and the data reduction procedures
to recover resolved disk images in Sect. 2, analyze the data in
Sect. 3, discuss our findings in Sect. 4, and conclude this study
in Sect. 5.

**2. Observation and data reduction**

We summarized a total of 23 systems observed in corona-
graphic imaging mode using both STIS (filter: 50CORON; λ<sub>c</sub> =
0.58 µm, pixel scale: 50.72 mas pixel<sup>-1</sup>, Riley et al. 2018) and
NICMOS Camera 2 (NIC2; filter: F110W or F160W; λ<sub>c</sub> =
1.12 µm or 1.60 µm, pixel scale: 75.65 mas pixel<sup>-1</sup>, Viana
et al. 2009). In Fig. 1, we display the transmission curves of
the three filters (obtained from Rodrigo et al. 2012; Rodrigo
& Solano 2020). The debris systems are 49 Ceti, AU Mic,
Beta Pic, HD 377, HD 15115, HD 15745, HD 30447, HD 32297,
HD 35650, HD 35841, HD 61005, HD 104860, HD 110058,
HD 131835, HD 141569A, HD 141943, HD 181327, HD 191089.
HD 192758, HD 202917, HR 4796A, TWA 7, and TWA 25. We
summarize the properties<fnref n="1" /> of the targets in Table 1, and the
exposure information in Table A.1.

2.1. Space telescope imaging spectrograph

Using STIS, we observed four systems (HD 30447, HD 35841,
HD 141943, and HD 191089) under HST GO-13381² (PI:
M. Perrin) and nine systems (49 Ceti, HD 377, HD 35650,
HD 104860, HD 110058, HD 131835, HD 192758, TWA 7, and
TWA 25) under HST GO-15218³ (PI: É. Choquet). From the
MAST archive,<fnref n="4" /> we retrieved six systems (AU Mic, HD 15115,
HD 15745, HD 32297, HD 61005, and HD 181327) from HST

<footnote n="1">¹ Unless otherwise specified, the error bars calculated in this paper are 1σ.</footnote>

<footnote n="2">² https://www.stsci.edu/cgi-bin/get-proposal-info?id=13381&observatory=HST</footnote>

<footnote n="3">³ https://www.stsci.edu/cgi-bin/get-proposal-info?id=15218&observatory=HST</footnote>

<footnote n="4">⁴ https://archive.stsci.edu</footnote>
<figure><img src="image_2.png" /><figcaption>Fig. 1. Transmission of the STIS-50CORON, NIC2-F110W, and NIC2-F160W coronagraphic filters used to image debris disks in this study.</figcaption></figure>

GO-12228 (PI: G. Schneider; Schneider et al. 2014) and two systems (HD 202917 and HR 4796A) from HST GO-13786 (PI: G. Schneider; Schneider et al. 2016, 2018). For Beta Pic, we retrieved its observations from three programs: SM2/ERO-7125 (PI: S. Heap; Heap et al. 2000), HST GO-12551 (PI: D. Apai; Apai et al. 2015), and HST GO-12923 (PI: A. Gaspar; Schneider et al. 2017). For HD 141569A, from three programs: HST GO-8624 (PI: A. Weinberger), HST GO-8674 (PI: A.-M. Lagrange; Mouillet et al. 2001), and HST GO-13786 (PI: G. Schneider; Konishi et al. 2016).

For each target, we reduced the observation data with multi-roll combined PSF template subtraction (MRDI: Schneider et al. 2014) using its corresponding PSF reference images designated in each HST program. We note that although HD 377 was previously observed in HST GO-12291 (PI: J. Krist), it was not recovered since the major axis of the disk coincides with either the STIS occulter or the diffraction spikes. In addition, we observed negligible differences between median-combined and mean-combined images, and thus we used the mean-combined MRDI images for a proper propagation of errors. We present the reduced images in Fig. 2.

## 2.2. NICMOS

We assembled the NICMOS observations for the targets and their corresponding PSF references from the Archival Legacy Investigations of Circumstellar Environments (ALICE) project<fnref n="5" /> (PI: R. Soummer; Choquet et al. 2014; Hagan et al. 2018). We reduced the data with the non-negative matrix factorization method (NMF; Ren et al. 2018) using 30% of the most correlated references with 50 sequentially constructed NMF components. To recover the true surface brightness of these disks, we adopted a forward modeling approach assuming simple geometric models for debris architecture (Augereau et al. 1999) and analytical SPFs (e.g., Henyey & Greenstein 1941). Due to the high computational cost of NMF component calculation (Ren et al. 2018), we saved the components computed in data reduction for subsequent forward modeling. We present the reduced images in Figs. 3 and 4 for filters F110W and F160W, respectively.

As opposed to the classical PSF subtraction method used for the STIS observations where there are dedicated stable reference star images, the NMF algorithm used for NICMOS, which was

shown to be able to better extract faint signals with higher quality than previous methods (e.g., Ren et al. 2018, 2021), still introduces certain levels of overfit of disk signals. This is due to the diversity in stellar types, instrument observing conditions, and image stability in archival NICMOS observations, which makes the reference images not able to fully capture target PSFs for all observations in the near-infrared. To recover the surface brightness of a NICMOS disk, we did not adopt the scaling factor in Ren et al. (2018) that requires stable PSFs. Instead, we estimated the throughput of the algorithm by performing forward modeling to capture the PSF variation in the NICMOS archive. Specifically, we adopted the Millar-Blanchaer et al. (2015) code to create a disk model whose dust particles follow analytical SPFs in Henyey & Greenstein (1941), and modified them in our study.

To depict the spatial geometry of a debris disk, we used the Ren et al. (2021) modification of the Millar-Blanchaer et al. (2015) code: a combined power law in the disk mid-plane, and a vertical Gaussian dispersion (see Augereau et al. 1999). In cylindrical coordinates the disk follows

$$ \rho(r, z) \propto \left[ \left( \frac{r}{r_c} \right)^{-2\alpha_{\text{in}}} + \left( \frac{r}{r_c} \right)^{-2\alpha_{\text{out}}} \right]^{-\frac{1}{2}} \exp \left[ - \left( \frac{z}{hr} \right)^2 \right], \quad (1) $$

where $r_c$ is the critical radius, $\alpha_{\text{in}} > 0$ and $\alpha_{\text{out}} < 0$ are the asymptotic power law indices when $r \ll r_c$ and $r \gg r_c$, respectively. Although the scale height parameter is $h = 0.04$ from a theoretical study by Thébault (2009), we note that edge-on disks may deviate from this value, and thus retrieve it in our disk modeling procedure. To account for the inner and outer clearing radii beyond which there are no dust particles, $r_{\text{in}}$ and $r_{\text{out}}$, we only evaluate Eq. (1) when $r_{\text{in}} < r < r_{\text{out}}$, and it equals 0 otherwise. To depict the SPF of the scatterers in a debris disk, we adopted a two-component Henyey-Greenstein function (e.g., Chen et al. 2020) since the original analytical phase function in Henyey & Greenstein (1941) is monotonous; however, that monotonicity is not always observed in actual debris disk observations (e.g., Stark et al. 2014; Chen et al. 2020).

For each target, we first generated a model disk image, then convolved it with the corresponding NICMOS point source PSF created by TinyTim (Krist et al. 2011)<fnref n="6" /> using the effective temperature of the star from Table 1. We subtracted the convolved disk from the observations to perform again the NMF reduction using the originally calculated NMF components to reduce computational cost. For the debris disks in this study, we did not see major differences on re-computing the NMF components; this is likely due to the fact that the PSF wings are sufficiently brighter than debris disks in the data analyzed here, thus the latter do not contribute significantly to the selection of best-matching reference images. In comparison, when circumstellar disks are brighter than PSF wings, we do indeed expect improvement of data reduction quality with NMF component re-computation (e.g., HD 100453 with VLT/SPHERE: Xie et al., in prep.).

We distributed the calculation and forward modeling process using DebrisDiskFM (Ren et al. 2019) on a computer cluster, and explored the parameter space with emcee (Foreman-Mackey et al. 2013). The best-fit models minimize the residuals by maximizing the log-likelihood,

$$ \ln \mathcal{L}(\mathbf{\Theta} | X_{\text{obs}}) = -\frac{1}{2} \sum_{i=1}^{N} \left( \frac{X_{\text{obs},i} - X_{\text{model},i}}{\sigma_{\text{obs},i}} \right)^2 - \sum_{i=1}^{N} \ln \sigma_{\text{obs},i} - \frac{N}{2} \ln(2\pi), \quad (2) $$

<footnote n="6">⁶ http://tinytim.stsci.edu</footnote>

<footnote n="5">⁵ https://archive.stsci.edu/prepds/alice/</footnote>
<table><caption>**Table 1.** Property of debris disk hosts observed by HST/STIS and HST/NICMOS.</caption><thead><tr><th>ID</th><th>Target</th><th>SpType</th><th>V<br>(mag)</th><th>Distance<br>(pc)</th><th>T<sub>eff</sub><br>(K)</th><th>M<sub>star</sub><br>(M<sub>☉</sub>)</th><th>L<sub>star</sub><br>(L<sub>☉</sub>)</th><th>log g<br>(cm s<sup>-2</sup>)</th><th>a<sub>BO</sub><br>(µm)</th><th colspan="2">Reference</th></tr><tr><th>(1)</th><th>(2)</th><th>(3)</th><th>(4)</th><th>(5)</th><th>(6)</th><th>(7)</th><th>(8)</th><th>(9)</th><th>(10)</th><th>SpType<br>(11)</th><th>V-mag<br>(12)</th></tr></thead><tbody><tr><td>a</td><td>49 Ceti</td><td>A1V</td><td>5.61</td><td>57.23<sup>+0.18</sup><sub>-0.18</sub></td><td>9000<sup>+170</sup><sub>-400</sub></td><td>2.2<sup>+0.3</sup><sub>-0.3</sub></td><td>15.7<sup>+0.7</sup><sub>-0.7</sub></td><td>4.32<sup>+0.07</sup><sub>-0.07</sub></td><td>2.5<sup>+0.4</sup><sub>-0.4</sub></td><td>1</td><td>13</td></tr><tr><td>b</td><td>AU Mic</td><td>M1V</td><td>8.63</td><td>9.714<sup>+0.002</sup><sub>-0.002</sub></td><td>3992<sup>+150</sup><sub>-166</sub></td><td>0.710<sup>+0.014</sup><sub>-0.014</sub></td><td>0.073<sup>+0.004</sup><sub>-0.004</sub></td><td>4.6<sup>+0.06</sup><sub>-0.06</sub></td><td>0.036<sup>+0.002</sup><sub>-0.002</sub></td><td>2</td><td>14</td></tr><tr><td>c</td><td>Beta Pic</td><td>A6V</td><td>3.86</td><td>19.63<sup>+0.06</sup><sub>-0.06</sub></td><td>7100<sup>+300</sup><sub>-300</sub></td><td>1.9<sup>+0.2</sup><sub>-0.2</sub><sup>(a)</sup></td><td>8.97<sup>+0.07</sup><sub>-0.07</sub><sup>(a)</sup></td><td>4.4<sup>+0.3</sup><sub>-0.3</sub><sup>(a)</sup></td><td>1.65<sup>+0.17</sup><sub>-0.17</sub></td><td>3</td><td>15</td></tr><tr><td>d</td><td>HD 377</td><td>G2V</td><td>7.59</td><td>38.40<sup>+0.04</sup><sub>-0.04</sub></td><td>5871<sup>+30</sup><sub>-40</sub></td><td>1.07<sup>+0.13</sup><sub>-0.13</sub></td><td>1.16<sup>+0.03</sup><sub>-0.03</sub></td><td>4.44<sup>+0.08</sup><sub>-0.08</sub></td><td>0.38<sup>+0.05</sup><sub>-0.05</sub></td><td>4</td><td>15</td></tr><tr><td>e</td><td>HD 15115</td><td>F4IV</td><td>6.80</td><td>48.77<sup>+0.07</sup><sub>-0.07</sub></td><td>6811<sup>+150</sup><sub>-150</sub></td><td>1.4<sup>+0.2</sup><sub>-0.2</sub></td><td>3.73<sup>+0.15</sup><sub>-0.15</sub></td><td>4.31<sup>+0.08</sup><sub>-0.08</sub></td><td>0.90<sup>+0.15</sup><sub>-0.15</sub></td><td>5</td><td>16</td></tr><tr><td>f</td><td>HD 15745</td><td>F0</td><td>7.49</td><td>71.73<sup>+0.12</sup><sub>-0.12</sub></td><td>6840<sup>+130</sup><sub>-140</sub></td><td>1.5<sup>+0.3</sup><sub>-0.3</sub></td><td>4.21<sup>+0.17</sup><sub>-0.17</sub></td><td>4.27<sup>+0.09</sup><sub>-0.09</sub></td><td>1.0<sup>+0.18</sup><sub>-0.18</sub></td><td>6</td><td>16</td></tr><tr><td>g</td><td>HD 30447</td><td>F3V</td><td>7.86</td><td>80.31<sup>+0.14</sup><sub>-0.14</sub></td><td>6709<sup>+130</sup><sub>-150</sub></td><td>1.5<sup>+0.3</sup><sub>-0.3</sub></td><td>3.73<sup>+0.14</sup><sub>-0.14</sub></td><td>4.31<sup>+0.09</sup><sub>-0.09</sub></td><td>0.89<sup>+0.16</sup><sub>-0.16</sub></td><td>7</td><td>16</td></tr><tr><td>h</td><td>HD 32297</td><td>A6V</td><td>8.14</td><td>129.7<sup>+0.5</sup><sub>-0.5</sub></td><td>7980<sup>+170</sup><sub>-80</sub></td><td>1.9<sup>+0.3</sup><sub>-0.3</sub></td><td>8.5<sup>+0.4</sup><sub>-0.4</sub></td><td>4.36<sup>+0.08</sup><sub>-0.08</sub></td><td>1.5<sup>+0.3</sup><sub>-0.3</sub></td><td>8</td><td>16</td></tr><tr><td>i</td><td>HD 35650</td><td>K6V</td><td>9.05</td><td>17.461<sup>+0.005</sup><sub>-0.005</sub></td><td>4175<sup>+150</sup><sub>-60</sub></td><td>0.66<sup>+0.08</sup><sub>-0.08</sub></td><td>0.129<sup>+0.009</sup><sub>-0.009</sub></td><td>4.6<sup>+0.11</sup><sub>-0.11</sub></td><td>0.069<sup>+0.010</sup><sub>-0.010</sub></td><td>4</td><td>17</td></tr><tr><td>j</td><td>HD 35841</td><td>F3V</td><td>8.90</td><td>103.07<sup>+0.14</sup><sub>-0.14</sub></td><td>6305<sup>+200</sup><sub>-80</sub></td><td>1.3<sup>+0.2</sup><sub>-0.2</sub></td><td>2.43<sup>+0.10</sup><sub>-0.10</sub></td><td>4.38<sup>+0.09</sup><sub>-0.09</sub></td><td>0.64<sup>+0.11</sup><sub>-0.11</sub></td><td>1</td><td>16</td></tr><tr><td>k</td><td>HD 61005</td><td>G8V</td><td>8.22</td><td>36.45<sup>+0.02</sup><sub>-0.02</sub></td><td>5507<sup>+60</sup><sub>-120</sub></td><td>0.97<sup>+0.12</sup><sub>-0.12</sub></td><td>0.636<sup>+0.014</sup><sub>-0.014</sub></td><td>4.54<sup>+0.07</sup><sub>-0.07</sub></td><td>0.23<sup>+0.03</sup><sub>-0.03</sub></td><td>3</td><td>16</td></tr><tr><td>l</td><td>HD 104860</td><td>G0/F9V</td><td>7.91</td><td>45.19<sup>+0.04</sup><sub>-0.04</sub></td><td>5939<sup>+60</sup><sub>-100</sub></td><td>1.11<sup>+0.15</sup><sub>-0.15</sub></td><td>1.18<sup>+0.04</sup><sub>-0.04</sub></td><td>4.48<sup>+0.08</sup><sub>-0.08</sub></td><td>0.37<sup>+0.05</sup><sub>-0.05</sub></td><td>9</td><td>16</td></tr><tr><td>m</td><td>HD 110058</td><td>A0V</td><td>7.97</td><td>130.1<sup>+0.5</sup><sub>-0.5</sub></td><td>8039<sup>+900</sup><sub>-190</sub></td><td>2.0<sup>+0.3</sup><sub>-0.3</sub></td><td>9.4<sup>+0.5</sup><sub>-0.5</sub></td><td>4.4<sup>+0.08</sup><sub>-0.08</sub></td><td>1.6<sup>+0.3</sup><sub>-0.3</sub></td><td>10</td><td>16</td></tr><tr><td>n</td><td>HD 131835</td><td>A2IV</td><td>7.86</td><td>129.7<sup>+0.5</sup><sub>-0.5</sub></td><td>8266<sup>+500</sup><sub>-300</sub></td><td>2.1<sup>+0.3</sup><sub>-0.3</sub></td><td>10.9<sup>+0.9</sup><sub>-0.9</sub></td><td>4.37<sup>+0.08</sup><sub>-0.08</sub></td><td>1.8<sup>+0.3</sup><sub>-0.3</sub></td><td>7</td><td>16</td></tr><tr><td>o</td><td>HD 141569</td><td>A2V</td><td>7.12</td><td>111.6<sup>+0.4</sup><sub>-0.4</sub></td><td>8439<sup>+200</sup><sub>-700</sub></td><td>2.1<sup>+0.4</sup><sub>-0.4</sub></td><td>15.3<sup>+4.0</sup><sub>-4.0</sub></td><td>4.2<sup>+0.3</sup><sub>-0.3</sub></td><td>2.5<sup>+0.8</sup><sub>-0.8</sub></td><td>11</td><td>16</td></tr><tr><td>p</td><td>HD 141943</td><td>G2</td><td>7.97</td><td>60.14<sup>+0.08</sup><sub>-0.08</sub></td><td>5673<sup>+100</sup><sub>-110</sub></td><td>1.09<sup>+0.14</sup><sub>-0.14</sub></td><td>2.07<sup>+0.06</sup><sub>-0.06</sub></td><td>4.22<sup>+0.08</sup><sub>-0.08</sub></td><td>0.66<sup>+0.09</sup><sub>-0.09</sub></td><td>4</td><td>17</td></tr><tr><td>q</td><td>HD 181327</td><td>F6V</td><td>7.04</td><td>47.78<sup>+0.07</sup><sub>-0.07</sub></td><td>6436<sup>+40</sup><sub>-160</sub></td><td>1.3<sup>+0.2</sup><sub>-0.2</sub></td><td>2.88<sup>+0.11</sup><sub>-0.11</sub></td><td>4.3<sup>+0.08</sup><sub>-0.08</sub></td><td>0.76<sup>+0.13</sup><sub>-0.13</sub></td><td>4</td><td>16</td></tr><tr><td>r</td><td>HD 191089</td><td>F5V</td><td>7.18</td><td>50.11<sup>+0.05</sup><sub>-0.05</sub></td><td>6450<sup>+50</sup><sub>-180</sub></td><td>1.3<sup>+0.2</sup><sub>-0.2</sub></td><td>2.74<sup>+0.10</sup><sub>-0.10</sub></td><td>4.33<sup>+0.09</sup><sub>-0.09</sub></td><td>0.72<sup>+0.12</sup><sub>-0.12</sub></td><td>7</td><td>16</td></tr><tr><td>s</td><td>HD 192758</td><td>F0V</td><td>7.03</td><td>66.50<sup>+0.14</sup><sub>-0.14</sub></td><td>7200<sup>+160</sup><sub>-200</sub></td><td>1.6<sup>+0.3</sup><sub>-0.3</sub></td><td>5.4<sup>+0.2</sup><sub>-0.2</sub></td><td>4.26<sup>+0.09</sup><sub>-0.09</sub></td><td>1.2<sup>+0.2</sup><sub>-0.2</sub></td><td>10</td><td>19</td></tr><tr><td>t</td><td>HD 202917</td><td>G7V</td><td>8.67</td><td>46.71<sup>+0.03</sup><sub>-0.03</sub></td><td>5506<sup>+70</sup><sub>-100</sub></td><td>0.98<sup>+0.12</sup><sub>-0.12</sub></td><td>0.668<sup>+0.016</sup><sub>-0.016</sub></td><td>4.53<sup>+0.08</sup><sub>-0.08</sub></td><td>0.24<sup>+0.03</sup><sub>-0.03</sub></td><td>4</td><td>19</td></tr><tr><td>u</td><td>HR 4796A</td><td>A0V</td><td>5.77</td><td>70.8<sup>+0.2</sup><sub>-0.2</sub></td><td>9670<sup>+100</sup><sub>-500</sub></td><td>2.5<sup>+0.3</sup><sub>-0.3</sub></td><td>24.7<sup>+1.1</sup><sub>-1.1</sub></td><td>4.35<sup>+0.06</sup><sub>-0.06</sub></td><td>3.5<sup>+0.5</sup><sub>-0.5</sub></td><td>7</td><td>16</td></tr><tr><td>v</td><td>TWA 7</td><td>M2V</td><td>10.91</td><td>34.10<sup>+0.03</sup><sub>-0.03</sub></td><td>4018<sup>+150</sup><sub>-170</sub></td><td>0.46<sup>+0.09</sup><sub>-0.09</sub></td><td>0.115<sup>+0.019</sup><sub>-0.019</sub></td><td>4.18<sup>+0.17</sup><sub>-0.17</sub></td><td>0.09<sup>+0.02</sup><sub>-0.02</sub></td><td>4</td><td>16</td></tr><tr><td>w</td><td>TWA 25</td><td>M0.5</td><td>11.16</td><td>53.60<sup>+0.07</sup><sub>-0.07</sub></td><td>4020<sup>+200</sup><sub>-160</sub></td><td>0.60<sup>+0.08</sup><sub>-0.08</sub></td><td>0.23<sup>+0.02</sup><sub>-0.02</sub></td><td>4.17<sup>+0.13</sup><sub>-0.13</sub></td><td>0.14<sup>+0.02</sup><sub>-0.02</sub></td><td>12</td><td>17</td></tr></tbody></table>

**Notes.** Column (1): Letter identifiers of the targets in this paper. Column (2): Target name. Column (3): Spectral type from the literature (Col. 11). Column (4): V-band magnitude from the literature studies in Col. (12). Column (5): Distance computed from Gaia DR3 parallaxes (Gaia Collaboration 2022). Column (6): Effective temperature from Gaia DR2 (Gaia Collaboration 2018). Values in Col. (7) for star mass, Col. (8) for stellar luminosity, and Col. (9) for stellar surface gravity are from the *Transiting Exoplanet Survey Satellite* input catalog (Stassun et al. 2018). Column (10): Expected dust blow-out size for nonporous amorphous olivine using Eq. (5). While M stars do not have sufficient radiation pressure to blow out small dust (e.g., Arnold et al. 2019), we report the corresponding blow-out sizes for color–size correlation analysis in Sect. 4.2. (a) For Beta Pic, the uncertainties of $M_{star}$, $L_{star}$, and log g are scaled from David & Hillenbrand (2015), Anders et al. (2019), and Gaia Collaboration (2018), respectively. If the upper and lower uncertainties are different, the bigger one is adopted.

**References.** In Columns (11) and (12), the references are for spectral type and V-mag, respectively: (1) Houk & Smith-Moore (1988); (2) Keenan & McNeil (1989); (3) Gray et al. (2006); (4) Torres et al. (2006); (5) Harlan (1974); (6) Cannon & Pickering (1993); (7) Houk (1982); (8) Rodigas et al. (2014); (9) Kahraman Aliçavuş et al. (2016); (10) Houk (1978); (11) Gray et al. (2017); (12) Herczeg & Hillenbrand (2014); (13) Høg et al. (2000); (14) Kiraga (2012); (15) Ducati (2002); (16) Wenger et al. (2000); (17) Zacharias et al. (2012).

where N is the number of pixels, σ is the uncertainty, and we assume that the pixels i follow independent normal distributions, with $X_{obs}$ and $X_{model}$ denoting the observation and model datasets, respectively. To quantify the uncertainty, we first obtained the algorithmic throughput of the best-fit model by comparing the model with the NMF reduction, then performed uncertainty measurement on the original individual NMF reductions with throughput correction.

## 2.3. Data for joint analysis

Given that the observed debris disks are of different inclinations, and that scatterers in debris disk systems redistribute incident light to different directions with varying intensity via SPFs (e.g., Stark et al. 2014; Milli et al. 2017), we measured the light with a scattering angle of ≈90° to minimize such effects to enable a uniform comparison of different systems. We used the regions annotated in Appendix A.2 for measurements on the signal and background for both instruments. Specifically for NICMOS, by comparing our reduction of the original dataset

with the best-fit convolved disk model, we can quantify the algorithmic throughput from the NMF post-processing procedure by dividing the NMF-reduced data with the best-fit model. We performed photometry on originally reduced data, subtracted flat halo backgrounds, and corrected the throughput measured from forward modeling. By doing so rather than performing measurements on the best-fit models, we expect to better capture the minor variations in observed disk signals.

We obtained the regions for birth ring photometry and halo background measurements as follows. Using the HD 181327 system as an example, we first identified the debris birth ring in Fig. A.1(q) using the ring parameters (e.g., semimajor axis, position angle, inclination) from Stark et al. (2014), then calculated for each pixel its scattering angle and associated angle uncertainty assuming an infinitely thin disk following Ren et al. (2019, Appendix A therein). To identify the pixels that host birth ring signals, if a pixel’s $1\sigma$ range of scattering angles overlaps with the [80°, 100°] interval, we categorize it as a birth ring pixel with a scattering angle of ≈90°. To reduce certain contributions
<figure><img src="image_3.png" /><figcaption>**Fig. 2.** Surface brightness distribution of the STIS disks. The color bars are in log scale with arbitrary units to adjust for differences in disk surface brightness across our debris disk gallery, and the scale bars are 50 au.</figcaption></figure>

from the halo signals, we chose the pixels that are 1.5 times the distance of the birth ring from the star for HD 181327, and calculated their mean for a flat halo background removal in further steps. To further assess the variation of halo background at different locations surrounding HD 181327, we measured the halo background at distinct locations with varying region areas (while avoiding known birth ring signals), and we observed no significant difference from the measured trends in Sect. 3.

For all debris systems, as a result, removing flat halo backgrounds induced minor deviations on the birth ring signals

regardless of the location of the background pixels since halos can be one or two orders of magnitude fainter than the birth rings (e.g., Schneider et al. 2014, 2018; Ren et al. 2019, 2021). The detected STIS halos in Fig. 2 and in the NICMOS images are only evident in log scale display. Halo background removal in linear scale, as well as the variation of halo signals within the chosen regions, has a minor influence (<0.5σ) on the extracted birth ring signals or the trend of birth ring color in Sect. 3.

We also note that for nearly edge-on systems (e.g., AU Mic, Beta Pic, HD 32297, HD 141943) where we performed
<figure><img src="image_4.png" /><figcaption>**Fig. 3.** Surface brightness distribution of the NICMOS disks using the F110W filter. The color bars are in log scale with arbitrary units, and the scale bars are 50 au.</figcaption></figure>

measurements on the ansae of the debris disks, the measure-
ments can actually probe a range of scattering angles that can
deviate significantly from ≈90°. To explore possible measure-
ment biases for these targets, as well as the impact of internal
halo flat background at different regions for all targets, we varied
the areas of regions for analysis for all systems by increas-
ing or decreasing the signal and background extraction areas in
Appendix A.2 by factors of up to 4 either individually or jointly,
and we did not observe statistically significant changes in our
results or their interpretation in this study. We therefore adopt
the regions identified in Appendix A.2 for further analysis on
both birth ring color and flat halo background removal.

3. Analysis

We computed the STIS–NICMOS color of the disk images as
follows. We first computed the reflectance in different filters for
each system, then obtained the color for them.

3.1. *Reflectance*

We obtained the instrument response<sup>7</sup> for the stars in units
of Jy by calculating the unobstructed instrumental response

<footnote n="7">7 The instrument response in this study refers to stellar flux density integrated in the instrument filters unless otherwise specified.</footnote>
<figure><img src="image_5.png" /><figcaption>**Fig. 4.** Surface brightness distribution of the NICMOS disks using the F160W filter. The color bars are in log scale with arbitrary units, and the scale bars are 50 au.</figcaption></figure>

to the Kurucz (1993) star models using pysynphot (STScI Development Team 2013), where the inputs are their effective temperature (*T*<sub>eff</sub>), V-band magnitude, and surface gravity (log *g*) in Table 1. For NICMOS F110W and NICMOS F160W, the parameter is ‘nicmos,2,f110w’ and ‘nicmos,2,f160w’, respectively. For STIS it is ‘stis,ccd,a2d4’.<fnref n="8" /> We summarized the instrument response of the two coronagraphs in Table A.1.

For the pre- and post-NCS eras of NICMOS operation (i.e., Era 1 and Era 2, respectively; see, e.g., Schultz et al. 2003) where

the sensitivities of the instrument are distinct, we adopted different PHOTFNU values to convert instrument counts to physical units of Jansky. For the two eras the PHOTFNU parameter for F110W is 1.84724 × 10<sup>-6</sup> and 2.03470 × 10<sup>-6</sup>, respectively. For F160W it is 1.21121 × 10<sup>-6</sup> and 1.49585 × 10<sup>-6</sup>. The pysynphot values correspond to Era 2 observations; for Era 1 observations we thus first multiplied an instrument count rate by the PHOTFNU value in Era 2, then divided it by the PHOTFNU value in Era 1, to obtain the count rate in Era 1. For each image, we obtained the fraction of light reflected by the debris disk via dividing the calibrated image by the pysynphot rates for the star. We used these fraction images for color analysis.

<footnote n="8">⁸ https://pysynphot.readthedocs.io/en/latest/appendixb.html</footnote>
## 3.2. Dust color

To obtain the STIS–NICMOS color for a disk, we averaged 2 × 2 NICMOS pixels (1 NICMOS pixel is 75.65 mas) into 1 bin, and 3 × 3 STIS pixels (1 STIS pixel is 50.72 mas) into 1 bin, with each bin being a square of approximately 150 mas in length. We then divided the binned STIS image by the square of the ratio of the width of the STIS bin (152.16 mas) to that of the NICMOS bin (153.3 mas) to account for spatial scale difference, and converted the fraction values to magnitudes. To compare the reflectance in the two wavelengths for dust color, we subtracted the NICMOS magnitude from the STIS magnitude. In this way, a positive STIS–NICMOS value means the disk scatters more light in NICMOS than in STIS (i.e., a red scatterer), while taking into account of the effect in the intrinsic brightness of the host star at different wavelengths.

We computed the ansae color along the major axes of the disks (i.e., a scattering phase angle of ≈90° between the incident light and the reflected light rays) to minimize the dependence of scattering intensity as a function of scattering phase angles (SPFs; e.g., Hedman & Stark 2015). A discussion on the contributions of signals from unbound particles (i.e., flat halo background) and the regions used for their removal can be found in Sect. 4.1 (see Appendix A.2 for the regions used for color extraction and background removal).

We present the dust color at the ansae of the birth rings as a function of stellar luminosity, obtained from Stassun et al. (2018) in Fig. 5. Comparing STIS with NICMOS observations, we note that the general color is blue, while it becomes more neutral when stellar luminosity increases. In comparison with existing debris disk color studies comparing STIS and NICMOS (e.g., Ren et al. 2019, 2021), the observed colors are consistent within $2\sigma$ despite different color extraction methods. Nevertheless, for HR 4796A in STIS and F110W, although Debes et al. (2008) and Rodigas et al. (2015) obtained red colors for the entire disk and the ansae, respectively, their results could have been compromised by the fact that certain signals were previously regarded as background before Schneider et al. (2018, Fig. 9 therein) and then removed. A blue ansae color measured for HR 4796A in this study is instead in agreement with the simulations from Thebault & Kral (2019), where the authors expected blue colors for debris birth rings for all A-type stars.

We observe that the F110W and F160W observations have a nearly neutral color, as well as a marginal trend with stellar luminosity in Fig. 5. A neutral color within the NICMOS wavelengths could arise from multiple aspects. First, the two NICMOS filters are adjacent to each other in wavelength in Fig. 1, which might not provide distinctive differences from dust properties. Second, the NICMOS data were observed under less stable instrument conditions than STIS; although the NMF data reduction and forward modeling steps had outperformed other classical or statistics-based methods in the results, the results are still dominated by instrument instability or incomplete reference image sampling in NICMOS observations. Last but not least, the sample size of debris disks observed in these filters are smaller than when they are compared with STIS observations. Due to these aspects, we do not further discuss the trustworthiness of the color results within NICMOS wavelengths or their implications here.

## 3.3. Color–albedo distribution: 90° scattering albedo

In planetary science studies on Solar System minor objects (e.g., asteroids, comets, and zodiacal light), spectral gradient and albedo can show different properties of these objects. The

<figure><img src="image_6.png" /></figure>

**Fig. 5.** Dust color at 80°–100° scattering angle as a function of stellar luminosity. The letters next to the color bars are the letter identifiers for the targets in Table 1. Panels a and b suggest that dust particles scatter light more efficiently at shorter wavelengths for less luminous stars. Although the trend in panel c does not agree with the other two, it is marginal and likely impacted by smaller sample size and data reduction artifacts. The shaded areas are $1\sigma$, $2\sigma$, and $3\sigma$ confidence bands from bootstrapping fit. See Table A.2 for the color values.

normalized reflectivity gradient follows $S' = \frac{1}{S} \frac{dS}{dl}$, where S is the reflectance at wavelength $\lambda$, and $\bar{S}$ is the average reflectance (e.g., Yang & Ishiguro 2015). Under this convention, positive $S'$ indicates that the scatterers are more efficient in scattering photons in longer wavelengths, defined as a red color in our study (see Figs. 1 and 6 in Yang & Ishiguro 2015 for a comparison between zodiacal light, red color in their Fig. 6, and different asteroids).

Given that the measurement for an asteroid normally has a dominant scattering angle, while the resolved debris disks by HST have a range of scattering angles depending on their inclinations, we calculated a location-specific albedo for the debris disk samples in this study. Our definition of albedo is performed on the resolved debris disk only for those regions that satisfy one criterion, within which the scattering angles of the dust particles are between 80° and 100°.

### 3.3.1. Albedo measurements

In an observed disk image in Fig. 2, the area of regions with 90° ± 10° scattering angles can occupy a fraction
<figure><img src="image_7.png" /><figcaption>Fig. 6. Disk color and 90° scattering albedo distribution defined in Eq. (4). The likely L-shaped clustering of color-albedo distribution might resemble that of Solar System objects, which might indicate different formation history or composition of debris birth rings. See Table A.2 for the albedo values.</figcaption></figure>

$f_{[80^{\circ},100^{\circ}]} \in (0, 1]$ of the entire disk in the disk plane depending on the inclination of the disk: for a face-on disk, the entirety of the disk image has a 90° scattering angle; for an edge-on disk, only the on-sky ansae of the birth ring (rather than the entirety of the major axis) have ~90° scattering angles. To correct for this inclination-induced effect on the total scattered light at ~90° scattering angle, and to recover all the scattered light that is not fully captured by the telescope along our line of sight, our recovery of 90° scattering albedo follows

$$ \alpha_{[80^{\circ},100^{\circ}]} = \frac{\frac{F_{\text{disk}}/f_{[80^{\circ},100^{\circ}]}}{F_{\text{star}}}}{\frac{F_{\text{disk}}/f_{[80^{\circ},100^{\circ}]}}{F_{\text{star}}} + \frac{L_{\text{IR}}}{L_{\text{star}}}}, \quad (3) $$

$$ = \frac{\frac{F_{\text{disk}}}{F_{\text{star}}}}{\frac{F_{\text{disk}}}{F_{\text{star}}} + \frac{L_{\text{IR}}}{L_{\text{star}}} \times f_{[80^{\circ},100^{\circ}]}}}, \quad (4) $$

where the disk flux $F_{\text{disk}}$ is integrated in the observed disk region that satisfies the regional criteria. By recovering the entire region of scattered light in Eq. (3) using the partially observed data via $\frac{F_{\text{disk}}}{f_{[80^{\circ},100^{\circ}]}}$, it is equivalent to multiplying the infrared excess of the disk $\frac{L_{\text{IR}}}{L_{\text{star}}}$ by the fraction of the disk region in Eq. (4).

Using the debris ring surface brightness values from STIS, we present the color-albedo measurements in Fig. 6. For the infrared excess values, we adopted the infrared excess data for HD 141569 from Mawet et al. (2017) and the rest from Cotten & Song (2016). We note a likely L-shaped clustering of debris disk albedo and color for the samples. In comparison with Solar System objects, only B-type and some C-type asteroids, both of which are carbonaceous and belong to C-group asteroids (Tholen 1989), are blue, while other commonly observed S-type (siliceous) and X-type (metal-rich) asteroids are reddish (e.g., Yang & Ishiguro 2015; Mahlke et al. 2022).

### 3.3.2. Comparison with Solar System minor objects

In visible to near-infrared wavelengths, most of the icy Kuiper Belt objects are red (e.g., Tegler & Romanishin 2000; Jewitt & Luu 2001; Delsanti et al. 2006). Nevertheless, EL$_{61}$ group objects, which could have formed from a giant impact that removed ice mantles (e.g., Barkume et al. 2006; Brown et al. 2007), are slightly bluish (Merlin et al. 2007; Pinilla-Alonso et al. 2008). The EL$_{61}$ spectrum can be explained by a large amount of crystalline and amorphous water ice on the surface (Trujillo et al. 2007; Merlin et al. 2007). The albedos of Kuiper Belt objects, which are not necessarily measured at ~90° scattering angles as for debris disks in this study, have a large range from 0.01 to 0.8, with the majority of them below 0.2 (e.g., Fig. 3 of Stansberry et al. 2008). As for the Kuiper Belt dust, direct infrared observation is still not practical due to contamination of thermal emissions from the zodiacal cloud (Jewitt 2008; Brown 2012).

With an overarching caveat that the color-albedo studies on Solar System objects and on debris disks in Fig. 6 are on objects with distinct sizes (kilometer-sized objects and micrometer-sized particles, respectively), the color-albedo distribution of the debris disks here might qualitatively resemble some C-group asteroids and a very few Kuiper Belt objects (e.g., Yang & Ishiguro 2015, Fig. 1 therein). Nevertheless, given that the two albedos are calculated differently, although the debris disk albedos might resemble qualitatively most C-type asteroids and Kuiper Belt objects, it does not suggest that the debris disk dust is made of materials that are identical to these Solar System objects.

In the young Solar System, dynamical processes can mix the minor objects along the radial direction (DeMeo & Carry 2014). As a result, the current spatial locations of Solar System minor objects does not match their initial locations. Therefore, the colors of the planetary objects can change over time from mechanisms such as space weathering, in which high-energy particles from the Sun and cosmic rays bombard these minor objects (Hapke 2001) on a timescale shorter than 1 Myr (Vernazza et al. 2009; DeMeo et al. 2023). Space weathering could cause both the reddening (Binzel et al. 2001) and the bluing (Moroz et al. 2004) of minor objects, depending on the size of the grains (Thompson et al. 2020) and the composition (e.g., C-type asteroids become bluer while S-type ones become redder; Nesvorný et al. 2005). The color change mechanisms for Solar System minor objects could further complicate the implications for the ensemble properties for the measurements of debris disks in this study.

Among Solar System minor objects, Q-type asteroids are considered to have fresh surfaces, which could retain pristine materials that might resemble debris disk dust, and are composed of ordinary chondrites. However, Hasegawa et al. (2019) showed that the color of minor object spectra could be the consequence of space weathering on grains larger than 100 microns. Therefore, given that the measured colors of Solar System objects are likely on dust that are ~100 µm while the typical sizes of debris disk dust are ~1 µm in scattered light here, there might not be pristine materials on the surface of the current Solar System objects, and thus a direct comparison of the colors between debris disks and Solar System objects is not feasible. Although we cannot directly match debris disks with Solar System minor objects, the likely L-shaped color-albedo distribution of the debris disks in Fig. 6 might indicate not only the difference in dust composition, but also different (levels of) activities such as space weathering in the observed debris systems.
### 3.3.3. Debris disk color-albedo clustering

The likely L-shaped clustering of debris disk albedo and color in Fig. 6, in comparison with that of Solar System objects (with a caveat regarding the different definition of albedos), indicates that the dust particles in different debris disk systems are formed differently and/or have different compositions. Nevertheless, there is an extra source of physically motivated uncertainty for our measurements: the collisional simulation study by Thebault & Kral (2019) suggests that the halo outside the birth ring could contribute to ~50% of the flux up to ~50 µm.

The contribution from halo grains can impact infrared excess measurements (Thebault & Kral 2019), and consequently would bias the albedo values measured here; we assumed all the infrared excess, which is a combination from the birth ring and the halo, are from the debris ring in Eq. (3). Given that the infrared excess signal from the birth ring alone is not easily separable in the Thebault & Kral (2019) study, we also investigated a possible lower limit of that signal. Specifically, to explore the influence of halo grains on SEDs, we adopted the infrared excess of cold belts from Chen et al. (2014) in which the authors performed two-belt fits to the SEDs. By applying the Chen et al. (2014) cold belt results to Eq. (3) (with a caveat that the actual infrared excess could be lower; e.g., Thebault & Kral 2019), we only observed quantitative offsets for Fig. 6, and the different clusterings of color-albedo did not change qualitatively. However, recalling that two-belt SED fits still cannot intrinsically separate the contributions from the birth ring and the halo properly, the significant infrared excess contribution from halo grains in the Thebault & Kral (2019) study suggests that the actual albedo values should be different from those presented in Fig. 6.

## 4. Discussion

### 4.1. Blue color of debris disks

Comparing STIS and NICMOS observations of the debris disks in scattered light in ~0.6 µm and in ~1.1 µm or ~1.6 µm, we obtained a predominantly blue color at the ansae (≈90° scattering angle) of debris birth rings. The observed blue color can suggest the ubiquitous existence of the submicron-sized particles that scatter light more efficiently on shorter wavelengths than larger particles. The theoretical simulation study in Thebault & Kral (2019) did show that even for A-type stars that were previously expected to blow out submicron-sized dust, high fractional luminosity disks (≥10⁻³) surrounding them can still harbor a sufficient number of these unbound dust particles (Fig. 2 therein) that are enough to make debris disks appear blue in scattered light (Fig. 13 therein).

While we have identified certain halo background areas that could aid in reducing the impact of unbound particles, the predominantly blue color of debris disk birth rings suggests that submicron-sized particles are widespread in all the systems studied here. What is more, the observed predominantly blue color suggests that a simple flat background removal adopted here has limited impact on removing unbound dust contribution since contributions from the SPFs of unbound particles are not negligible, especially when there are enough such particles, as in Thebault & Kral (2019). Moreover, and more importantly, there are other factors that could make the removal of a flat halo background less practical. First, Lee & Chiang (2016) simulations have shown that the existence of eccentric planet(s) can perturb the surface density distribution of halo particles. Second, the regions that we used to measure halo background have different

stlocentric distances from that of the birth ring, requiring a distance-based illumination correction. Last but not least, the number density and surface density distributions of the unbound grains in the halo are not identical to that in the birth ring, calling for more investigations on the simulation results in or beyond Thebault & Kral (2019). Together with these limitations in removing the contribution from unbound particles on disk color measurement, a measurement of unbound particles in the debris halo is not necessarily representative of their contribution at other locations, including the birth ring. After all, the majority of debris disk birth rings are indeed blue, especially since submicron-sized particles, some of which are unbound when hosted by early-type stars, naturally reside in birth rings (e.g., Thebault & Kral 2019).

The blue debris ring color is more neutral for more luminous stars in Fig. 5. For the more luminous early-type stars, there could be a small but sufficient number of submicron-sized particles that are unbound to make the debris rings blue (Thebault & Kral 2019). In comparison, the less luminous later-type stars can indeed retain submicron-sized particles (e.g., Arnold et al. 2019), and these bound particles could make debris rings appear blue. As a result, for debris disks orbiting stars with increasing stellar luminosity in Fig. 5, the submicron-sized particles within can turn from bound to unbound (i.e., from M-type to A-type stars), making the disks more neutral. Although it is not feasible to completely remove the color contribution from unbound particles in this study, the general trend of the color being more neutral for more luminous stars, if true, could be in line with the expectation that less submicron-sized particles are bound for earlier type stars (see Sect. 4.2 for a correlation between color and expected blow-out size of dust particles).

Moving forward, to observationally better reveal the debris ring color for bound particles in debris systems (e.g., Fig. 13 of Thebault & Kral 2019, in which debris disks orbiting A-type stars turn from red to blue when unbound particles are taken into account), radiative transfer models of the SPFs for unbound particles are necessary to remove SPF effects at different scattering angles. Such modeling would be achieved in principle by fitting the observed halo intensity as a function of scattering angle, then by extrapolating the brightness for the unbound particles at debris birth ring regions. However, these models could be challenging in terms of dust morphological model, size, composition, and computational feasibility (e.g., Tazaki & Tanaka 2018; Tazaki et al. 2019; Arnold et al. 2019) since they should be more realistic in resembling interplanetary dust particles (IDPs), which are produced from asteroids or comets from the inner main asteroid belt to the Kuiper belt and they do have aggregate or fractal morphology (e.g., Bradley 2003). In addition, the Lee & Chiang (2016) simulations showed that the existence of hidden planetary perturber(s) on eccentric orbits can change the surface density distribution of particles in both the birth ring and the halo. We leave such an analysis on extracting debris birth ring colors only for bound particles for future studies.

### 4.2. Dust blow-out size and disk color

A dust particle experiences the force balance between radiational pressure and gravity pull, and it becomes unbound when the former exceeds the latter on an orbital timescale. For a given stellar system, we can calculate the dust blow-out size for nonporous dust using Eq. (5) of Arnold et al. (2019), while assuming the average radiation-pressure efficiency over the stellar spectrum to be unity for compact spheres. Substituting the values for spherical amorphous olivine particles which have a mass density of
3.3 g cm⁻³, as in Chen et al. (2014), we obtain

$$a_{BO} = 0.35 \mu m \times \frac{L_{star}}{M_{star}}, \qquad (5)$$

where L<sub>star</sub> and M<sub>star</sub> are in solar units (see Col. (10) of Table 1 for the corresponding dust blow-out size). We note that we ignored dependences on dust properties such as composition and porosity (e.g., Arnold et al. 2019) to obtain a systematic view of the size information.

We fit the measured dust color with blow-out size using a linear relationship. There are positive correlations between the STIS-NICMOS colors and dust blow-out size, or Δmag<sub>STIS-F110W</sub> = 0.12<sup>+0.05</sup><sub>-0.05</sub>a<sub>BO</sub> - 0.74<sup>+0.06</sup><sub>-0.06</sub> and Δmag<sub>STIS-F160W</sub> = 0.17<sup>+0.07</sup><sub>-0.07</sub>a<sub>BO</sub> - 0.85<sup>+0.12</sup><sub>-0.12</sub>, respectively. The positive correlations indicate that that larger dust scatters light more efficiently at longer wavelengths, and thus make a debris system redder.

Although there is a negative relationship between F110-F160W color and dust blow-out size, or Δmag<sub>F110W-F160W</sub> = -0.07<sup>+0.07</sup><sub>-0.08</sub>a<sub>BO</sub> - 0.15<sup>+0.16</sup><sub>-0.15</sub>, the statistical significance is tangential. Given that both F110W and F160W observations have undergone the forward modeling procedure, and that only 10 out of the 23 systems have observations in both filters, such a negative relationship is likely impacted by data reduction artifact and small sample size. Nevertheless, we conclude that on the one hand, it is not fully valid to assume single composition or ignore porosity to calculate the actual blow-out size for debris disk systems, and on the other hand, it is challenging to calculate dust color for adjacent filters when data reduction artifacts are non-negligible.

### 4.3. Disk infrared excess and disk color

We present the disk color dependence on fractional infrared excess (L<sub>IR</sub>/L<sub>star</sub>) in Fig. 7, with the infrared excess data from Sect. 3.3. We observe a trend that disks with higher fractional infrared excess are more neutral in color. Following theoretical studies in which infrared excess decreases over time (e.g., Wyatt et al. 2007; Löhne et al. 2008; Gáspár et al. 2013), this color trend might be correlated with disk evolutionary stage; however, such a trend has a caveat that the debris disk colors are already under steady state in theoretical simulation studies (e.g., Thebault & Kral 2019). What is more, the fractional infrared excess is positively correlated with stellar luminosity in the samples in this study, making it probable that the former is not contributing to the color trend in Fig. 7.

To minimize the stellar luminosity contribution in the color dependence on fractional infrared excess, it is necessary to fit and remove stellar luminosity effects using Fig. 5. However, with the high dispersion of the data in stellar luminosity for the systems in this study, as well as the fact that the samples in this study are not from a uniform survey, a proper removal of stellar luminosity influences for Fig. 7 is beyond the scope of this study.

## 5. Conclusion

By extracting the resolved debris disks using the HST coronagraphs in visible and near-infrared light (~0.6 µm, and ~1.1 µm or ~1.6 µm) using classical reference differential imaging and forward modeling in the STIS and NICMOS coronagraphs, we obtained the reflectance of these debris disks in scattered light. We observe that the color of these disks is predominantly blue, which suggests that the dust particles in these systems scatter

<figure><img src="image_8.png" /><figcaption>Fig. 7. Dust color as a function of fractional infrared excess. Panels a, b, and c are for STIS-F110W, STIS-F160W, and F110W-F160W, respectively. With a caveat that infrared excess and stellar luminosity are positively correlated in Sect. 4.3, there might be marginal trends of the STIS-NICMOS color being more neutral for disks with higher fractional infrared excess.</figcaption></figure>

shorter-wavelength light more efficiently than longer-wavelength light.

In the color-albedo distribution of these systems, we note the clustering of scatterers that could qualitatively resemble the clustering of Solar System objects, albeit with different definitions of albedos adopted. What is more, a qualitative resemblance does not indicate a compositional similarity. Were such a clustering true for debris disks, it could indicate different formation history and compositions for these debris systems.

The dust particles in these systems scatter relatively efficiently (rather than absolutely more efficiently) in longer wavelengths, as the luminosity of the host star increases. This correlates with the expectation that more luminous stars can blow out larger dust particles, and thus can shift the dust color toward the redder direction. Nevertheless, given that there could still be a
large amount of submicron-sized unbound particles even in A-type stars (Thebault & Kral 2019), the measured blue color can arise from unbound particles in early-type stars as well as bound particles in late-type stars, which makes it challenging to separate these two kinds of contributions. A proper modeling and separation of scattered light contribution from unbound particles in the future is thus necessary to probe the birth ring color for bound particles in debris disks.

Accurate representation of the observed color and color-albedo distributions in debris disk systems requires the use of physically motivated dust models. In comparison with existing attempts with Mie scatterers or a distribution of hollow spheres encountering difficulties in explaining observations (e.g., Milli et al. 2019; Ren et al. 2019; Chen et al. 2020; Arriaga et al. 2020), Olofsson et al. (2022) successfully reproduced the polarized light observations of HD 32297 with the Tazaki & Tanaka (2018) models. The use of more sophisticated or realistic models (e.g., Arnold et al. 2019; Tazaki et al. 2019; Tobon Valencia et al. 2022) or lab measurements (e.g., Muñoz et al. 2021) to resemble the IDPs that originate from the asteroid belt and the Kuiper Belt will be necessary to properly depict the observed color and albedo for circumstellar disks in future works.

**Acknowledgements.** We thank the anonymous referee for their comments that increased the clarity, depth, and width of this paper. We thank Xinyu Lu and Marco Delbo for helpful discussions. This work was funded by NASA through STScI Grant # HST-GO-15218.014-A for HST GO-15218 program (PI: É. Choquet). We are grateful for the productive discussions about dust scattering properties as part triggered by the EPOPEE (Etude des POussières Planétaires Et Exoplanétaires) collaboration, supported by the French Planetology National Program (Programme National de Planétologie, PNP) of CNRS/INSU co-funded by CNES. We thank in particular Jean-Charles Augereau for helpful discussions about minimum grain sizes in debris disks and Jérémy Lasue for inspiring discussions about the diversity and properties of Solar System dust. E.C. acknowledges funds from CNRS/PICS TACO-DESIRE program for supporting this research. This project has received funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation programme (PROTOPLANETS, grant agreement No. 101002188), and under the European Union's Horizon Europe research and innovation programme (ESCAPE, grant agreement No. 101044152). Based on observations made with the NASA/ESA Hubble Space Telescope, obtained from the data archive at the Space Telescope Science Institute. STScI is operated by the Association of Universities for Research in Astronomy, Inc. under NASA contract NAS 5-26555. This research has made use of data reprocessed as part of the ALICE program, which was supported by NASA through grants HST-AR-12652 (PI: R. Soummer), HST-GO-11136 (PI: D. Golimowski), HST-GO-13855 (PI: É. Choquet), HST-GO-13331 (PI: L. Pueyo), and STScI Director's Discretionary Research funds, and was conducted at STScI which is operated by AURA under NASA contract NAS5-26555. This research has made use of the SIMBAD database (Wenger et al. 2000), operated at CDS, Strasbourg, France. This research has made use of the VizieR catalogue access tool, CDS, Strasbourg, France (DOI: 10.26093/cds/vizier). The original description of the VizieR service was published in A&AS 143, 23 (Ochsenbein et al. 2000). This research has made use of the SVO Filter Profile Service (http://svo2.cab.inta-csic.es/theory/fps/) supported from the Spanish MINECO through grant AYA2017-84089. The input images to ALICE processing are from the recalibrated NICMOS data products produced by the Legacy Archive project, "A Legacy Archive PSF Library And Circumstellar Environments (LAPLACE) Investigation," (HST-AR-11279, PI: G. Schneider). This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. Part of the computations presented here were conducted in the Resnick High Performance Computing Center, a facility supported by Resnick Sustainability Institute at the California Institute of Technology.

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# Appendix A: Supplementary materials

## A.1. Exposure information of targets

We summarize the exposure time information for the targets in Table A.1.

## A.2. Color extraction locations

We display the regions used to extract color information for the dust in Fig. A.1.

## A.3. Color and albedo values

We present the extracted color and albedo values in Table A.2.
<table><caption>**Table A.1.** Exposure time and instrument response for debris disk hosts</caption><thead><tr><th colspan="2">Instrument</th><th>F110W</th><th>F160W</th><th>STIS</th><th colspan="3">Instrument Response (Jy)</th></tr><tr><th>id<br>(1)</th><th>Target<br>(2)</th><th>(3)</th><th>Exposure Time (s)<br>(4)</th><th>(5)</th><th>(6)</th><th>(7)</th><th>(8)</th></tr></thead><tbody><tr><td>a</td><td>49 Ceti</td><td>2335.57</td><td>...</td><td>1918.8</td><td>11.0</td><td>...</td><td>16.3</td></tr><tr><td>b</td><td>AU Mic</td><td>2687.53</td><td>2687.53</td><td>13050</td><td>5.45</td><td>7.65</td><td>1.48</td></tr><tr><td>c</td><td>Beta Pic</td><td>127.78<sup>a</sup></td><td>47.92<sup>a</sup></td><td>2575.8</td><td>85.7</td><td>60.8</td><td>83.3</td></tr><tr><td>d</td><td>HD 377</td><td>4319.38</td><td>...</td><td>4596.6</td><td>4.08</td><td>...</td><td>2.76</td></tr><tr><td>e</td><td>HD 15115</td><td>4607.27</td><td>...</td><td>11484.8</td><td>6.21</td><td>...</td><td>5.59</td></tr><tr><td>f</td><td>HD 15745</td><td>1407.76</td><td>...</td><td>17730</td><td>3.26</td><td>...</td><td>2.96</td></tr><tr><td>g</td><td>HD 30447</td><td>1343.76</td><td>...</td><td>4320</td><td>2.41</td><td>...</td><td>2.11</td></tr><tr><td>h</td><td>HD 32297</td><td>1343.76</td><td>1343.76</td><td>13228.2</td><td>1.29</td><td>0.832</td><td>1.58</td></tr><tr><td>i</td><td>HD 35650</td><td>...</td><td>1503.57</td><td>6055.8</td><td>...</td><td>4.11</td><td>0.939</td></tr><tr><td>j</td><td>HD 35841</td><td>1343.76</td><td>...</td><td>4350</td><td>1.05</td><td>...</td><td>0.816</td></tr><tr><td>k</td><td>HD 61005</td><td>4607.34</td><td>...</td><td>13284</td><td>2.65</td><td>...</td><td>1.57</td></tr><tr><td>l</td><td>HD 104860</td><td>5183.26</td><td>...</td><td>6360</td><td>2.97</td><td>...</td><td>2.05</td></tr><tr><td>m</td><td>HD 110058</td><td>2303.6</td><td>2303.6</td><td>4708.8</td><td>1.49</td><td>0.956</td><td>1.84</td></tr><tr><td>n</td><td>HD 131835</td><td>2303.6</td><td>2303.6</td><td>4672.5</td><td>1.57</td><td>0.981</td><td>2.04</td></tr><tr><td>o</td><td>HD 141569</td><td>1215.76<sup>a</sup></td><td>863.5<sup>a</sup></td><td>16005.6</td><td>2.98</td><td>1.83</td><td>4.03</td></tr><tr><td>p</td><td>HD 141943</td><td>4607.34</td><td>1535.56</td><td>4479.6</td><td>3.09</td><td>2.74</td><td>1.95</td></tr><tr><td>q</td><td>HD 181327</td><td>1535.69</td><td>...</td><td>12812</td><td>5.58</td><td>...</td><td>4.51</td></tr><tr><td>r</td><td>HD 191089</td><td>4607.34</td><td>...</td><td>7847.6</td><td>4.89</td><td>...</td><td>3.97</td></tr><tr><td>s</td><td>HD 192758</td><td>3455.41</td><td>3455.41</td><td>4078.8</td><td>4.49</td><td>3.14</td><td>4.48</td></tr><tr><td>t</td><td>HD 202917</td><td>3519.51</td><td>1407.74<sup>a</sup></td><td>14034</td><td>1.75</td><td>1.62</td><td>1.04</td></tr><tr><td>u</td><td>HR 4796A</td><td>1951.65<sup>a</sup></td><td>2367.57<sup>a</sup></td><td>9525.6</td><td>8.72</td><td>5.05</td><td>14.2</td></tr><tr><td>v</td><td>TWA 7</td><td>...</td><td>1215.76<sup>a</sup></td><td>6718.8</td><td>...</td><td>0.953</td><td>0.177</td></tr><tr><td>w</td><td>TWA 25</td><td>...</td><td>1503.57</td><td>14508</td><td>...</td><td>0.755</td><td>0.141</td></tr></tbody></table>

**Notes:** Column (1): Letter identifiers of targets. Column (2): Target name. Columns (3), (4), and (5): Exposure time using F110W, F160W, and STIS, respectively. Columns (6), (7), and (8): *pysynphot* instrumental response for the unocculted stars using F110W, F160W, and STIS, respectively, with three significant digits.

<footnote><sup>a</sup>Observed in NICMOS Era 1.</footnote>
<figure><img src="image_9.png" /><figcaption>**Fig. A.1.** Regions used for dust color extraction (at 80°–100° scattering angle) and background removal overlayed onto STIS images. The surface brightness distributions of the disks are presented in log scale. Changing the area of either or both regions by up to a factor of 4 does not cause significant variation in the observed trends for color and albedo.</figcaption></figure>
<table><caption>**Table A.2.** Color and albedo information measured in this study</caption><thead><tr><th>id<br>(1)</th><th>Target<br>(2)</th><th>STIS-F110W<br>(3)</th><th>STIS-F160W<br>(4)</th><th>F110W-F160W<br>(5)</th><th>albedo(STIS-F110W)<br>(6)</th></tr></thead><tbody><tr><td>a</td><td>49 Ceti</td><td>-0.28<sup>+0.12</sup><sub>-0.12</sub></td><td>...</td><td>...</td><td>0.0165<sup>+0.0009</sup><sub>-0.0008</sub></td></tr><tr><td>b</td><td>AU Mic</td><td>-0.7<sup>+0.05</sup><sub>-0.05</sub></td><td>-0.5<sup>+0.05</sup><sub>-0.05</sub></td><td>-0.2<sup>+0.07</sup><sub>-0.07</sub></td><td>0.135<sup>+0.008</sup><sub>-0.008</sub></td></tr><tr><td>c</td><td>Beta Pic</td><td>-0.48<sup>+0.04</sup><sub>-0.04</sub></td><td>-0.661<sup>+0.015</sup><sub>-0.015</sub></td><td>0.19<sup>+0.04</sup><sub>-0.04</sub></td><td>0.0175<sup>+0.0004</sup><sub>-0.0004</sub></td></tr><tr><td>d</td><td>HD 377</td><td>-1.51<sup>+0.09</sup><sub>-0.09</sub></td><td>...</td><td>...</td><td>0.0175<sup>+0.0015</sup><sub>-0.0014</sub></td></tr><tr><td>e</td><td>HD 15115</td><td>-0.69<sup>+0.09</sup><sub>-0.09</sub></td><td>...</td><td>...</td><td>0.018<sup>+0.003</sup><sub>-0.003</sub></td></tr><tr><td>f</td><td>HD 15745</td><td>-0.67<sup>+0.11</sup><sub>-0.11</sub></td><td>...</td><td>...</td><td>0.081<sup>+0.007</sup><sub>-0.007</sub></td></tr><tr><td>g</td><td>HD 30447</td><td>-0.8<sup>+0.3</sup><sub>-0.3</sub></td><td>...</td><td>...</td><td>0.063<sup>+0.006</sup><sub>-0.006</sub></td></tr><tr><td>h</td><td>HD 32297</td><td>-0.57<sup>+0.08</sup><sub>-0.08</sub></td><td>-0.74<sup>+0.13</sup><sub>-0.13</sub></td><td>0.18<sup>+0.15</sup><sub>-0.15</sub></td><td>0.0073<sup>+0.0013</sup><sub>-0.0011</sub></td></tr><tr><td>i</td><td>HD 35650</td><td>...</td><td>-0.27<sup>+0.19</sup><sub>-0.19</sub></td><td>...</td><td>0.052<sup>+0.005</sup><sub>-0.005</sub></td></tr><tr><td>j</td><td>HD 35841</td><td>-0.22<sup>+0.18</sup><sub>-0.18</sub></td><td>...</td><td>...</td><td>0.039<sup>+0.009</sup><sub>-0.007</sub></td></tr><tr><td>k</td><td>HD 61005</td><td>-0.6<sup>+0.04</sup><sub>-0.04</sub></td><td>...</td><td>...</td><td>0.044<sup>+0.005</sup><sub>-0.004</sub></td></tr><tr><td>l</td><td>HD 104860</td><td>0.1<sup>+0.3</sup><sub>-0.3</sub></td><td>...</td><td>...</td><td>0.019<sup>+0.002</sup><sub>-0.002</sub></td></tr><tr><td>m</td><td>HD 110058</td><td>-0.1<sup>+0.3</sup><sub>-0.3</sub></td><td>-0.2<sup>+0.4</sup><sub>-0.4</sub></td><td>0.2<sup>+0.5</sup><sub>-0.5</sub></td><td>0.038<sup>+0.013</sup><sub>-0.010</sub></td></tr><tr><td>n</td><td>HD 131835</td><td>-1.0<sup>+0.6</sup><sub>-0.6</sub></td><td>-1.0<sup>+0.7</sup><sub>-0.7</sub></td><td>-0.0<sup>+0.9</sup><sub>-0.9</sub></td><td>0.025<sup>+0.003</sup><sub>-0.002</sub></td></tr><tr><td>o</td><td>HD 141569</td><td>-0.2<sup>+0.3</sup><sub>-0.3</sub></td><td>0.30<sup>+0.10</sup><sub>-0.10</sub></td><td>-0.5<sup>+0.3</sup><sub>-0.3</sub></td><td>0.0123<sup>+0.0016</sup><sub>-0.0014</sub></td></tr><tr><td>p</td><td>HD 141943</td><td>-1.16<sup>+0.12</sup><sub>-0.12</sub></td><td>-1.47<sup>+0.09</sup><sub>-0.09</sub></td><td>0.31<sup>+0.15</sup><sub>-0.15</sub></td><td>0.099<sup>+0.016</sup><sub>-0.014</sub></td></tr><tr><td>q</td><td>HD 181327</td><td>-0.93<sup>+0.03</sup><sub>-0.03</sub></td><td>...</td><td>...</td><td>0.187<sup>+0.004</sup><sub>-0.004</sub></td></tr><tr><td>r</td><td>HD 191089</td><td>-0.74<sup>+0.11</sup><sub>-0.11</sub></td><td>...</td><td>...</td><td>0.234<sup>+0.013</sup><sub>-0.012</sub></td></tr><tr><td>s</td><td>HD 192758</td><td>-0.9<sup>+0.4</sup><sub>-0.4</sub></td><td>-0.9<sup>+0.5</sup><sub>-0.5</sub></td><td>0.0<sup>+0.6</sup><sub>-0.6</sub></td><td>0.064<sup>+0.005</sup><sub>-0.005</sub></td></tr><tr><td>t</td><td>HD 202917</td><td>-0.31<sup>+0.13</sup><sub>-0.13</sub></td><td>-0.6<sup>+0.3</sup><sub>-0.3</sub></td><td>0.3<sup>+0.5</sup><sub>-0.3</sub></td><td>0.022<sup>+0.007</sup><sub>-0.005</sub></td></tr><tr><td>u</td><td>HR 4796A</td><td>-0.35<sup>+0.02</sup><sub>-0.02</sub></td><td>-0.31<sup>+0.04</sup><sub>-0.04</sub></td><td>-0.04<sup>+0.04</sup><sub>-0.04</sub></td><td>0.065<sup>+0.004</sup><sub>-0.004</sub></td></tr><tr><td>v</td><td>TWA 7</td><td>...</td><td>-1.27<sup>+0.14</sup><sub>-0.14</sub></td><td>...</td><td>0.57<sup>+0.02</sup><sub>-0.02</sub></td></tr><tr><td>w</td><td>TWA 25</td><td>...</td><td>-0.8<sup>+0.6</sup><sub>-0.6</sub></td><td>...</td><td>...</td></tr></tbody></table>

**Notes:** Column (1): Letter identifiers of the targets in this paper. Column (2): Target name. Column (3): STIS - F110W color. Column (4): STIS - F160W color. Column (5): F110W - F160W color. Column (6): 90° scattering albedo for STIS-F110W color.