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HST/WFC3 Imaging and Mul4-‐Wavelength Characteriza4on of Edge-‐On Protoplanetary Disks

Authors: Carolina “Cee” Gould1, Gaspard Duchene1,3, Karl Stapelfeldt2, Francois Menard3, Deborah Padgett4, Marchall D. Perrin5, Christophe Pinte3, Schuyler Wolff 6

Affilia4ons: 1. UC Berkeley, 2. NASA JPL, , 3. Université Grenoble Alpes, 4. NASA GSFC, , 5. STScI, 6. Johns Hopkins University Cee Gould Undergraduate, UC Berkeley

Duchene et al. 2002 A&A 400 559 Duchene et al. 2010 ApJ 712 112 McCabe et al. 2011 ApJ 727 90 Stapelfeldt et al. 1998 ApJL 502 L65 Watson et al. 2007 Protostars and Planets V p.523

Detailed Analysis of SSTTau J024021.4+281349

2MASS J11160287-‐7624533 HH 30

Results

Graph: Normalized surface brightness vs distance from the midplane. Similar results are obtained if the slice is taken at a different loca4on of the disk, so long as the jet is avoided.

Future

Acknow

ledgem

ents

•  Recently, in some disks we have iden.fied the presence of a tenuous “atmosphere” well above the disk midplane that we tenta.vely explain as due to small dust grains being li=ed up by magne.c and/or radia.ve forces.

•  Here we report on our effort to beder characterize such atmospheres and to search for correla4ons with other key parameters, such as the degree of disk sedling and the apparent intensity of ouelow ac4vity in the system.

•  We have obtained Cycle 22 deep HST/WFC3 F475W (λc = 0.48μm) images of 6 edge on disks, which are complimented by archival HST images at other visible wavelengths.

•  If small dust grains are responsible for the atmosphere, we expect them to sca@er much more efficiently at the shortest wavelengths and, thus, the atmosphere to be more prominent in the F475W images.

Goals

Metho

ds

This project has been supported by funding from the Space Telescope Science Ins4tute as part of program GO-‐13643. I would also like to give thanks the UCB SURF Program for providing the funding and resources to con4nue this research this summer.

HK Tau B

•  One of the key steps toward planet forma4on is the sedling of dust par4cles in the midplane of a protoplanetary disk. To study this, we need to characterize the ver4cal structure of a number of disks. •  Edge-‐on disks provide a unique observing opportunity as the glare of the bright central star is blocked by the disk itself and the ver.cal structure of the disk is in direct view (e.g. Watson et al. 2007) •  For many years, our team has combined high resolu4on (HST and adap4ve op4cs) images of of edge-‐on protoplanetary disks and high fidelity radia4ve transfer models to extract the key physical parameters of each disk (e.g. Stapelfeldt et al. 1998; Duchene et al. 2004, 2010; McCabe et al. 2011). Co

ntext

Here we present preliminary results, including 3-‐color visible light images of all disks, which were made using only HST observa4ons (WFPC2, ACS, and/or WFC3) and with the filters F475W, F606W, and F814W. Included is the well-‐studied HH 30 system, and a more detailed analysis of the largest edge-‐on disk system in our sample.

Objects

Name SFR RDisk SpT Jet Disk Atmosphere

1 2 3 4 5 6

7

#

2MASS J11160287-‐7624533

SSTGBS J111110.7-‐764157

HK Tau B

2MASS J16281370-‐2431391

HH 30

SSTC2D J163131.2-‐242627

SSTTau J024021.4+281349

1

2

3

4

5

6

7 Tau 450 AU M1 Flared ✔ ✔

Oph 160 AU M ✗ ✗ Flat/Sedled

✔

✔

✔

✔

✗

✗

✗

Flared ✔

Flared

Flat/Sedled

Flat/Sedled

Flared

105 AU Tau

✔

(Lep) HST 3 color F814W, F606W, and F475W: (Center) 3 color HST and Keck F814W, J, K’ : (Right) HST 2 color F606W and F814W and CARMA 1.3mm contours

Future work will include quan4fying the observed atmosphere and disentangling it from the disk, which will involve radia4ve transfer modeling. We will then search to correlate the appearance of an atmosphere with other disk proper4es, including presence of a jet, mass, and degree of sedling as an indicator of evolu4on.

The plot on the right maps the surface brightness along the disk. This plot was created by first aligning the filtered images, then isola4ng a slice along the disk, at the loca4on illustrated by the red line along the disk in the inset. The curve was then created by mapping the intensity of each pixel along the length of the slice. From the graph, we see that the intensity of surface brightness drops faster at longer, redder, wavelengths (K’) as a func4on of distance away from the midplane. Conversely, our new pursuit of the bluer F475W profile further captures this trend: the intensity of surface brightness drops slower at shorter, bluer, wavelengths. This observa4on that there is s4ll blue light at large distances from the disk then strongly suggests the presence of small dust grains in this region.

A range of targets were selected to emphasize disk diversity, as there is no obvious correla4on between a visible atmosphere and stellar or other disk characteris4cs. Moving forward, possible correla4ons with other system proper4es such as X-‐ray luminosity will be explored.

Interes4ng to note the silhouede in disk #4 in the F475W image, i.e., absorp4on of background emission by the opaque disk itself, as there is evidence for a similar phenomenon at mm wavelength for the same system.

225 AU Tau

[email protected]

Cha

Cha

Oph 300 AU

125 AU

75 AU

✗

M0

M

M2

M2.5

K8

References

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SSTGBS J111110.7-‐764157 2MASS J16281370-‐2431391 SSTC2D J163131.2-‐242627