Astrochemical Modeling of Infrared Dark Clouds
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Examensarbete för masterexamen
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Sammanfattning
Infrared Dark Clouds (IRDCs) are cold, dense regions of the interstellar medium
(ISM) that are likely to represent the initial conditions for massive star and star
cluster formation. It is thus important to study the physical and chemical conditions
of IRDCs to provide constraints and inputs for theoretical models of these
processes. We aim to determine the astrochemical conditions, especially cosmic ray
ionization rate (CRIR) and chemical age, in different regions of the massive IRDC
G28.37+00.07 by comparing observed abundances of multiple molecules and molecular
ions with the predictions of astrochemical models. We have computed a series
of single-zone, time-dependent, astrochemical models with a gas-grain network that
systematically explores the parameter space of density, temperature, CRIR, and visual
extinction. We have also investigated the effects of choices of CO ice binding
energy and temperatures achieved in transient heating of grains when struck by
cosmic rays. We selected 10 positions across the IRDC that are known to have a
variety of star formation activity. We utilised mid-infrared (MIR) extinction maps
and sub-mm emission maps to measure the mass surface densities of these regions,
needed for abundance and volume density estimates. The sub-mm emission maps
were also used to measure temperatures. We then used IRAM-30m observations of
various tracers, especially C18O(1-0), H13CO+(1-0), HC18O+(1-0), and N2H+(1-0),
to estimate column densities and thus abundances. Finally, we investigated the
range of astrochemical conditions that are consistent with the observed abundances.
Results: The typical physical conditions of the IRDC regions are nH ∼ 3 × 104 to
105 cm−3 and T ≃ 10 to 15 K. Strong emission of H13CO+(1-0) and N2H+(1-0) is
detected towards all the positions and these species are used to define relatively
narrow velocity ranges of the IRDC regions, which are used for estimates of CO
abundances, via C18O(1-0). CO depletion factors are estimated to be in the range
fD ∼ 3 to 10. Using estimates of the abundances of CO, HCO+ and N2H+ we find
consistency with astrochemical models that have relatively low CRIRs of ζ ∼ 10−18
to ∼ 10−17 s−1, with no evidence for systematic variation with the level of star formation
activity. Astrochemical ages, defined with reference to an initial condition
of all H in H2, all C in CO, and all other species in atomic form, are found to be
< 1 Myr. We also explore the effects of using other detected species, i.e., HCN,
HNC, HNCO, CH3OH, and H2CO, to constrain the models. These generally lead
to implied conditions with higher levels of CRIRs and older chemical ages. Considering
the observed fD versus nH relation of the 10 positions, which we find to have
relatively little scatter, we discuss potential ways in which the astrochemical models
can match such a relation as a quasi-equilibrium limit valid at ages of at least a few
free-fall times, i.e., ≳ 0.3 Myr, including the effect of CO envelope contamination,
small variations in temperature history near 15 K, CO-ice binding energy uncertainties
and CR induced desorption. We find general consistency with the data of
∼ 0.5 Myr-old models that have ζ ∼ 2 − 5 × 10−18 s−1 and CO abundances set by a
balance of freeze-out with CR induced desorption.
Conclusions: We have constrained the astrochemical conditions in 10 regions in
a massive IRDC, finding evidence for relatively low values of CRIR compared to
diffuse ISM levels. We have not seen clear evidence for variation in the CRIR with
the level of star formation activity. We favour models that involve relatively low
CRIRs (≲ 10−17 s−1) and relatively old chemical ages (≳ 0.3 Myr, i.e., ≳ 3tff). We
discuss potential sources of systematic uncertainties in these results and the overall
implications for IRDC evolutionary history and astrochemical models.
Beskrivning
Ämne/nyckelord
astrochemistry, molecular clouds, star formation