Accretion Rates as a Diagnostic Tool for the Origin of Planetary-mass Companions

Thank you! 867686264 Assigned ID: 965 ----- Attempting Submission 1 (Fri Mar 06 23:57:45 GMT 2020) ----- Each orbit of Visit 6 is trimmed by 150 sec. -1637928287 ----- Attempting Submission 1 (Mon Jun 29 05:39:51 GMT 2020) ----- ----- Attempting Submission 2 (Thu Jul 16 18:58:49 GMT 2020) ----- HST Phase II Proposal 16302 successfully submitted. Receipt: # 16302-2 ----- Attempting Submission 3 (Thu Oct 15 08:01:58 GMT 2020) ----- ----- Attempting Submission 4 (Wed Oct 21 17:46:34 GMT 2020) ----- ----- Attempting Submission 5 (Wed Dec 02 13:01:45 GMT 2020) ----- ----- Attempting Submission 6 (Tue Dec 15 12:49:48 GMT 2020) ----- ----- Attempting Submission 7 (Sun Jan 16 17:18:03 GMT 2022) ----- FLASH values are ~20. Accretion Rates as a Diagnostic Tool for the Origin of Planetary-mass Companions Direct imaging surveys have revealed a new population of substellar companions with masses around the deuterium burning limit and orbits often farther than 100 AU. The formation of these planetary-mass companions (PMCs) is not fully understood. While core/pebble accretion and dynamical scattering seem unlikely, disk fragmentation and prestellar core collapse remain to be tested. Simulations have shown that disk fragmentation generally leads to higher mass accretion rates than prestellar core collapse. Therefore, PMCs are expected to have higher accretion rates than free-floating planets/brown dwarfs if disk fragmentation is the dominant formation channel. Alternatively, if both populations have indistinguishable accretion rates, that would suggest a common origin. To test this prediction, we propose to observe the UV continuum excess and H-alpha emission for PMCs and free-floating objects with WFC3/UVIS multi-band imaging. Our targets are of comparable mass and age, and have evidence indicative of disks. We will carry out shock modeling and search for any population-level accretion rate differences between the two samples. We will also investigate the empirical relationship between H-alpha line luminosities and accretion luminosities from the stellar-mass toward the planetary-mass regime, in order to establish whether the mass assembly process for stars, brown dwarfs, and planetary-mass objects are analogous and continuous. We propose to measure the intensity of H-alpha emission and the UV/optical spectral energy distribution between 2000 A and 8000 A for 5 wide-orbit planetary-mass companions and 8 free-floating planets/brown dwarfs, with the narrow-band filter F656N for H-alpha and 6 wide-band filters for the accretion-induced continuum excess (F225W, F336W, F438W, F555W, F625W, F775W). The observed fluxes are expected to predominantly originate from the accretion continuum as the photospheric emission from young planetary-mass objects is faint in the optical. The exposure times are chosen to reach a sensitivity level of 10^-19 erg/s/cm^2/A in all wide-band filters, ensuring that we can readily detect the photosphere of a ~10 Jupiter-mass object at wavelengths longer than 5000 A: 2000 s for F225W, 500 s for F336W, 500 s for F438W, 150 s for F555W, 120 s for F625W, and 150 s for F775W. Our photometric sensitivity corresponds to a mass accretion rate of 10^-13 Msun/yr based on Robinson & Espaillat (2019). The exposure time for F656N, 1200 s, will reach a rms of <10^-18 erg/s/cm^2/A, which is about the expected photospheric level at 6500 A and therefore ensures a very high S/N detection of H-alpha. To calculate the H-alpha line intensity, we will estimate the adjacent continuum by fitting atmospheric/accretion models to the observed F625W and F775W fluxes. The choice of F336W and F438W allows us to characterize the Balmer jump and help model the temperature and density of the accretion flow. The F225W filter is important to probe the peak of the UV continuum. We describe our observation sequence as follows. We will observe each target for two consecutive orbits, one orbit with the optical filters (F438W, F555W, F625W, F656N, F775W) and the other orbit with the UV filters (F225W, F336W). In total, we will use 26 orbits for this program (13 targets x 2 orbits/target). To minimize the overheads and avoid the lengthy pauses of reading out the instrument buffer, we will use the UVIS2-C512C-SUB subarray (513 x 512 pixels). Its field of view (~20") is large enough to simultaneously image the companions as well as the primary stars. We will adopt the 3-point dither pattern (WFC3-UVIS-DITHER-LINE-3PT) for the observations to efficiently remove cosmic rays. For observations of those 5 companions ([SCH06] J0359+2009 B, FU Tau B, CT Cha B, SR 12 c, CS Cha c), we also specify the acceptable ORIENT in order to minimize any impact from diffraction spikes and bleeding. Dr. Ya-Lin Wu's research focuses on multi-wavelength observations of substellar companions and circumstellar disks particularly using adaptive optics systems and ALMA. Dr. Brendan Bowler is a leading expert in direct observations of exoplanets with adaptive optics imaging and spectroscopy to study their statistical patterns, atmospheric properties, and formation mechanisms. Mr. Quang Tran is a graduate student working with Dr. Bowler to characterize exoplanet population demographics across different host properties. Dr. Yifan Zhou specializes in HST observations of variable brown dwarfs to study cloud dynamics and atmospheric compositions. Dr. Adam Kraus uses observations from the Hubble and Spitzer Space Telescopes, as well as large ground-based telescopes, to study the formation and evolution of planetary systems, including directly imaging gas giant planets as they form in orbit around other stars. Raquel Martinez is a graduate student working with Dr. Kraus on direct imaging of substellar companions with Spitzer to characterize the atmospheres in the mid-infrared. Dr. William Best is a leading expert in the demographics and atmospheres of brown dwarfs. He has also used HST and other ground-based infrared facilities to quantify the initial mass function in the substellar regime. Dr. Kimberly Ward-Duong has expertise working with multi-wavelength observations of low-mass stars and brown dwarfs and the direct imaging of substellar systems, and studied the circumstellar disk properties of objects across the substellar boundary, corresponding to the mass search space of the proposed sample. Dr. Katherine Follette is a leading expert in the field of direct imaging of accreting protoplanets and the search for young planets forming in transition disk systems. Dr. Catherine Espaillat is a leading expert in transitional disks and the accretion properties of young stellar systems, and has extensive experience working with HST data and simulating the accretion process. Mr. Connor Robinson is a graduate student working with Dr. Espaillat and has worked on novel approaches to modeling the accretion shocks in young, low-mass systems. Dr. Ian Czekala is an expert in the characterization of young stars through spectroscopy, working on multi-wavelength studies from the optical to the submillimeter to characterize star and planet formation processes. 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1642351981547 The scheduling data was generated by CASM 28.2. 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CASM was run in Phase II mode. 1633945690000 210.67206625619593 (Tic-Visit :proposal-id 16302 :visit-id "9B" :proposal-version -1 :trans-version "20200619" :date "15-Dec-2020 20:40:15.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 1 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 68656 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16302 :visit-id "9B" :obset-id "9B" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16302 :visit-id "9B" :orbit-number 1 :pcs-time 383 :si-vis-utilization 3136 :al-overhead-at-end 51 :internal-dur-at-end 112 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3519 :pcs-gap 0 ) true 1 0 1608036017565 The scheduling data was generated by CASM 28.2. CASM was run in Phase II mode. 1614444129000 353.1139970127944 (Tic-Visit :proposal-id 16302 :visit-id "10" :proposal-version -1 :trans-version "20200619" :date "15-Dec-2020 20:40:17.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 96112 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16302 :visit-id "10" :obset-id "10" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16302 :visit-id "10" :orbit-number 1 :pcs-time 383 :si-vis-utilization 3136 :al-overhead-at-end 51 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3519 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16302 :visit-id "10" :orbit-number 2 :pcs-time 392 :si-vis-utilization 3125 :al-overhead-at-end 48 :internal-dur-at-end 142 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3519 :pcs-gap 0 ) true 2 0 1608036019693 The scheduling data was generated by CASM 28.2. CASM was run in Phase II mode. 1613243205000 280.3511733894382 (Tic-Visit :proposal-id 16302 :visit-id "11" :proposal-version -1 :trans-version "20200619" :date "15-Dec-2020 20:40:19.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 96112 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16302 :visit-id "11" :obset-id "11" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16302 :visit-id "11" :orbit-number 1 :pcs-time 383 :si-vis-utilization 2773 :al-overhead-at-end 51 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3157 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16302 :visit-id "11" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2764 :al-overhead-at-end 49 :internal-dur-at-end 142 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3157 :pcs-gap 0 ) true 2 0 1608036021743 The scheduling data was generated by CASM 28.2. CASM was run in Phase II mode. 1612905754000 278.15764223124296 (Tic-Visit :proposal-id 16302 :visit-id "12" :proposal-version -1 :trans-version "20200619" :date "15-Dec-2020 20:40:21.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 96112 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16302 :visit-id "12" :obset-id "12" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16302 :visit-id "12" :orbit-number 1 :pcs-time 383 :si-vis-utilization 2773 :al-overhead-at-end 51 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3157 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16302 :visit-id "12" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2764 :al-overhead-at-end 49 :internal-dur-at-end 142 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3157 :pcs-gap 0 ) true 2 0 1608036023935 The scheduling data was generated by CASM 28.2. CASM was run in Phase II mode. 1613254734000 278.2236772480895 (Tic-Visit :proposal-id 16302 :visit-id "13" :proposal-version -1 :trans-version "20200619" :date "15-Dec-2020 20:40:23.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 96112 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 16302 :visit-id "13" :obset-id "13" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 16302 :visit-id "13" :orbit-number 1 :pcs-time 383 :si-vis-utilization 2773 :al-overhead-at-end 51 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3157 :pcs-gap 0 ) (Tic-Orbit :proposal-id 16302 :visit-id "13" :orbit-number 2 :pcs-time 392 :si-vis-utilization 2764 :al-overhead-at-end 49 :internal-dur-at-end 142 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3157 :pcs-gap 0 ) true 2 0