22 research outputs found
Spectral Line Analysis/Modeling (SLAM) I: pvanalysis
Line observations of young stellar objects (YSOs) at (sub)millimeter
wavelengths provide essential information of gas kinematics in star and planet
forming environments. For Class 0 and I YSOs, identification of Keplerian
rotation is of particular interest, because it reveals presence of
rotationally-supported disks that are still being embedded in infalling
envelopes and enables us to dynamically measure the protostellar mass. We have
developed a python library SLAM (Spectral Line Analysis/Modeling) with a
primary focus on analyses of emission line data at (sub)millimeter wavelengths.
Here, we present an overview of the pvanalysis tool from SLAM, which is
designed to identify Keplerian rotation of a disk and measure the dynamical
mass of a central object using a position-velocity (PV) diagram of emission
line data. The advantage of this tool is that it analyzes observational
features of given data and thus requires few computational time and parameter
assumptions, in contrast to detailed radiative transfer modelings. In this
article, we introduce the basic concept and usage of this tool, present an
application to observational data, and discuss remaining caveats.Comment: 13 pages, 8 figures, accepted for publication in PKA
Increasing mass-to-flux ratio from the dense core to the protostellar envelope around the Class 0 protostar HH 211
To study transportation of magnetic flux from large to small scales in
protostellar sources, we analyzed the Nobeyama 45-m N2H+ (1-0), JCMT 850 um
polarization, and ALMA C18O (2-1) and 1.3 mm and 0.8 mm (polarized) continuum
data of the Class 0 protostar HH 211. The magnetic field strength in the dense
core on a 0.1 pc scale was estimated with the single-dish line and polarization
data using the Davis-Chandrasekhar-Fermi method, and that in the protostellar
envelope on a 600 au scale was estimated from the force balance between the
gravity and magnetic field tension by analyzing the gas kinematics and magnetic
field structures with the ALMA data. Our analysis suggests that from 0.1 pc to
600 au scales, the magnetic field strength increases from 40-107 uG to 0.3-1.2
mG with a scaling relation between the magnetic field strength and density of
, and the mass-to-flux ratio increases from
1.2-3.7 to 9.1-32.3. The increase in the mass-to-flux ratio could suggest that
the magnetic field is partially decoupled from the neutral matter between 0.1
pc and 600 au scales, and hint at efficient ambipolar diffusion in the
infalling protostellar envelope in HH 211, which is the dominant non-ideal
magnetohydrodynamic effect considering the density on these scales. Thus, our
results could support the scenario of efficient ambipolar diffusion enabling
the formation of the 20 au Keplerian disk in HH 211.Comment: 27 pages, 12 figures, accepted by Ap
Early Planet Formation in Embedded Disks (eDisk). VIII. A Small Protostellar Disk around the Extremely Low-Mass and Young Class 0 Protostar, IRAS 15398-3359
Protostellar disks are a ubiquitous part of the star formation process and
the future sites of planet formation. As part of the Early Planet Formation in
Embedded Disks (eDisk) large program, we present high-angular resolution dust
continuum (mas) and molecular line (mas) observations of
the Class 0 protostar, IRAS 15398-3359. The dust continuum is small, compact,
and centrally peaked, while more extended dust structures are found in the
outflow directions. We perform a 2D Gaussian fitting to find the deconvolved
size and radius of the dust disk to be
and , respectively. We estimate the gas+dust disk mass
assuming optically thin continuum emission to be ,
indicating a very low-mass disk. The CO isotopologues trace components of the
outflows and inner envelope, while SO traces a compact, rotating disk-like
component. Using several rotation curve fittings on the PV diagram of the SO
emission, the lower limits of the protostellar mass and gas disk radius are
and from our Modified 2 single power-law
fitting. A conservative upper limit of the protostellar mass is inferred to be
. The protostellar mass-accretion rate and the specific angular
momentum at the protostellar disk edge are found to be between
and
, respectively, with an age
estimated between yr. At this young age with no clear
substructures in the disk, planet formation would likely not yet have started.
This study highlights the importance of high-resolution observations and
systematic fitting procedures when deriving dynamical properties of deeply
embedded Class 0 protostars.Comment: 28 pages, 16 figures. Accepted for publication in ApJ as one of the
first-look papers of the eDisk ALMA Large Progra
Early Planet Formation in Embedded Disks (eDisk) VI: Kinematic Structures around the Very Low Mass Protostar IRAS 16253-2429
Precise estimates of protostellar masses are crucial to characterize the
formation of stars of low masses down to brown-dwarfs (BDs; M* < 0.08 Msun).
The most accurate estimation of protostellar mass uses the Keplerian rotation
in the circumstellar disk around the protostar. To apply the Keplerian rotation
method to a protostar at the low-mass end, we have observed the Class 0
protostar IRAS 16253-2429 using the Atacama Large Millimeter/submillimeter
Array (ALMA) in the 1.3 mm continuum at an angular resolution of 0.07" (10 au),
and in the 12CO, C18O, 13CO (J=2-1), and SO (J_N = 6_5-5_4) molecular lines, as
part of the ALMA Large Program Early Planet Formation in Embedded Disks
(eDisk). The continuum emission traces a non-axisymmetric, disk-like structure
perpendicular to the associated 12CO outflow. The position-velocity (PV)
diagrams in the C18O and 13CO lines can be interpreted as infalling and
rotating motions. In contrast, the PV diagram along the major axis of the
disk-like structure in the 12CO line allows us to identify Keplerian rotation.
The central stellar mass and the disk radius are estimated to be ~0.12-0.17
Msun and ~13-19 au, respectively. The SO line suggests the existence of an
accretion shock at a ring (r~28 au) surrounding the disk and a streamer from
the eastern side of the envelope. IRAS 16253-2429 is not a proto-BD but has a
central stellar mass close to the BD mass regime, and our results provide a
typical picture of such very low-mass protostars.Comment: 41 pages, 14 figure
Early Planet Formation in Embedded Disks (eDisk) V: Possible Annular Substructure in a Circumstellar Disk in the Ced110 IRS4 System
We have observed the Class 0/I protostellar system Ced110 IRS4 at an angular
resolution of (10 au) as a part of the ALMA large program; Early
Planet Formation in the Embedded Disks (eDisk). The 1.3 mm dust continuum
emission reveals that Ced110 IRS4 is a binary system with a projected
separation of 250 au. The continuum emissions associated with the main
source and its companion, named Ced110 IRS4A and IRS4B respectively, exhibit
disk-like shapes and likely arise from dust disks around the protostars. The
continuum emission of Ced110 IRS4A has a radius of 110 au (),
and shows bumps along its major axis with an asymmetry. The bumps can be
interpreted as an shallow, ring-like structure at a radius of 40 au
() in the continuum emission, as demonstrated from two-dimensional
intensity distribution models. A rotation curve analysis on the CO and
CO -1 lines reveals the presence of a Keplerian disk within a
radius of 120 au around Ced110 IRS4A, which supports the interpretation that
the dust continuum emission arises from a disk. The ring-like structure in the
dust continuum emission might indicate a possible, annular substructure in the
surface density of the embedded disk, although the possibility that it is an
apparent structure due to the optically thick continuum emission cannot be
ruled out.Comment: 32 pages, 23 figures. Accepted for publication in ApJ as one of the
first-look papers of the eDisk ALMA Large Progra
Early Planet Formation in Embedded Disks (eDisk) III: A first high-resolution view of sub-mm continuum and molecular line emission toward the Class 0 protostar L1527 IRS
Studying the physical and chemical conditions of young embedded disks is
crucial to constrain the initial conditions for planet formation. Here, we
present Atacama Large Millimeter/submillimeter Array (ALMA) observations of
dust continuum at 0.06" (8 au) resolution and molecular line emission at
0.17" (24 au) resolution toward the Class 0 protostar L1527 IRS from the
Large Program eDisk (Early Planet Formation in Embedded Disks). The continuum
emission is smooth without substructures, but asymmetric along both the major
and minor axes of the disk as previously observed. The detected lines of
CO, CO, CO, HCO, c-CH, SO, SiO, and DCN trace
different components of the protostellar system, with a disk wind potentially
visible in CO. The CO brightness temperature and the HCO line
ratio confirm that the disk is too warm for CO freeze out, with the snowline
located at 350 au in the envelope. Both molecules show potential evidence
of a temperature increase around the disk-envelope interface. SO seems to
originate predominantly in UV-irradiated regions such as the disk surface and
the outflow cavity walls rather than at the disk-envelope interface as
previously suggested. Finally, the continuum asymmetry along the minor axis is
consistent with the inclination derived from the large-scale (100" or 14,000
au) outflow, but opposite to that based on the molecular jet and envelope
emission, suggesting a misalignment in the system. Overall, these results
highlight the importance of observing multiple molecular species in multiple
transitions to characterize the physical and chemical environment of young
disks.Comment: 27 pages, 16 figures, 2 tables, 10 pages appendix with 12 figures.
Accepted for publication in ApJ as one of the first-look papers of the eDisk
ALMA Large Progra
Early Planet Formation in Embedded Disks (eDisk). II. Limited Dust Settling and Prominent Snow Surfaces in the Edge-on Class I Disk IRAS 04302+2247
While dust disks around optically visible, Class II protostars are found to
be vertically thin, when and how dust settles to the midplane are unclear. As
part of the Atacama Large Millimeter/submillimeter Array (ALMA) large program,
Early Planet Formation in Embedded Disks, we analyze the edge-on, embedded,
Class I protostar IRAS 04302+2247, also nicknamed the ``Butterfly Star." With a
resolution of 0.05" (8~au), the 1.3 mm continuum shows an asymmetry along the
minor axis which is evidence of an optically thick and geometrically thick disk
viewed nearly edge-on. There is no evidence of rings and gaps, which could be
due to the lack of radial substructure or the highly inclined and optically
thick view. With 0.1" (16~au) resolution, we resolve the 2D snow surfaces,
i.e., the boundary region between freeze-out and sublimation, for CO
=2--1, CO =2--1, CO =2--1, CO
=--, and SO =--, and constrain the CO
midplane snow line to au. We find Keplerian rotation around a
protostar of using CO. Through forward
ray-tracing using RADMC-3D, we find that the dust scale height is au
at a radius of 100~au from the central star and is comparable to the gas
pressure scale height. The results suggest that the dust of this Class~I source
has yet to vertically settle significantly.Comment: 33 pages, 21 figures. Accepted for publication in ApJ as one of the
first-look papers of the eDisk ALMA Large Progra
Early Planet Formation in Embedded Disks (eDisk) XII: Accretion streamers, protoplanetary disk, and outflow in the Class I source Oph IRS63
We present ALMA observations of the Class I source Oph IRS63 in the context
of the Early Planet Formation in Embedded Disks (eDisk) large program. Our ALMA
observations of Oph IRS63 show a myriad of protostellar features, such as a
shell-like bipolar outflow (in CO), an extended rotating envelope
structure (in CO), a streamer connecting the envelope to the disk (in
CO), and several small-scale spiral structures seen towards the edge of
the dust continuum (in SO). By analyzing the velocity pattern of CO and
CO, we measure a protostellar mass of ~ and confirm the presence of a disk rotating at almost Keplerian
velocity that extends up to au. These calculations also show that the
gaseous disk is about four times larger than the dust disk, which could
indicate dust evolution and radial drift. Furthermore, we model the CO
streamer and SO spiral structures as features originating from an infalling
rotating structure that continuously feeds the young protostellar disk. We
compute an envelope-to-disk mass infall rate of ~ and compare it to the disk-to-star mass accretion rate of ~, from which we infer that the protostellar
disk is in a mass build-up phase. At the current mass infall rate, we speculate
that soon the disk will become too massive to be gravitationally stable.Comment: 26 pages and 17 figure
Early Planet Formation in Embedded Disks (eDisk). IV. The Ringed and Warped Structure of the Disk around the Class I Protostar L1489 IRS
Constraining the physical and chemical structure of young embedded disks is
crucial to understanding the earliest stages of planet formation. As part of
the Early Planet Formation in Embedded Disks Atacama Large
Millimeter/submillimeter Array Large Program, we present high spatial
resolution (0.\!\!^{\prime\prime}1 or 15 au) observations of the
1.3 mm continuum and CO 2-1, CO 2-1, and SO
- molecular lines toward the disk around the Class I protostar L1489
IRS. The continuum emission shows a ring-like structure at 56 au from the
central protostar and a tenuous, optically thin emission extending beyond
300 au. The CO emission traces the warm disk surface, while the
CO emission originates from near the disk midplane. The coincidence of
the radial emission peak of CO with the dust ring may indicate a
gap-ring structure in the gaseous disk as well. The SO emission shows a highly
complex distribution, including a compact, prominent component at 30
au, which is likely to originate from thermally sublimated SO molecules. The
compact SO emission also shows a velocity gradient along a slightly
() tilted direction with respect to the major axis of the dust
disk, which we interpret as an inner warped disk in addition to the warp around
200 au suggested by previous work. These warped structures may be formed
by a planet or companion with an inclined orbit, or by a gradual change in the
angular momentum axis during gas infall.Comment: 24 pages, 12 figures. Accepted for publication in The Astrophysical
Journal as one of the first-look papers of the eDisk ALMA Large Progra