Dark Clouds Research Articles

To the Editor: COVID-19 as a Catalyst to Transform Graduate Medical Education.

We applaud Wietlisbach and colleagues for highlighting the silver lining in the dark clouds of the COVID-19 pandemic.1 Their qualitative study based on 4 internal medicine (IM) residency programs in the Northeast United States suggests that IM residents adjusted quickly to the disruption and changes brought on by COVID-19 and focused on resiliency and well-being during the pandemic. Our own experience at a large IM residency program at Johns Hopkins Bayview Medical Center suggested that, although COVID-19 had a predominantly negative effect on the well-being of the residents, it also presented an incredible learning opportunity. Forty IM residents were contacted as part of a larger survey to monitor the stress and well-being of staff during COVID-19 at Johns Hopkins Bayview Medical Center between October and December 2020, out of which 18 (45%) completed the survey. Survey measures included Patient Health Questionnaire-2, Generalized Anxiety Disorder-7, and modified Maslach Burnout Inventory. In addition, residents were asked about the satisfaction of their educational experience.Survey results showed that 17% of the residents had significant depressive symptoms and sleep disturbances, while 25% endorsed moderate to severe anxiety symptoms. More than 70% residents felt burned out, and 22% indicated that they felt burned out and callous toward their work on a daily basis. Ninety-four percent of residents indicated that their training was significantly impacted by COVID-19. Sixty-seven percent had to miss their didactic training due to work demands. Thirty-three percent had to change their core or elective rotations. On the positive side, 50% of the residents indicated that they learned new skills during COVID-19 that contributed to their professional growth. Some of the comments from residents were: “Now on call as an intern,” “Taking on more shifts on my scheduled days off,” “Type of cases seen are limited by COVID,” “Zoom didactic sessions are not as effective as in person,” and “Less mentorship and teaching from upper residents and faculty.”In contrast to the Wietlisbach study, our survey suggests that the residents were less enthusiastic about the technological innovations in didactics and training and longed to go back to the pre-COVID-19 normal. However, we also found a strong focus of resiliency by the residents, with 61% of the sample scoring >6 on the 2-item Connor-Davidson Resilience Scale. We agree with Wietlisbach and colleagues that COVID-19 can be a catalyst in the transformation of graduate medical education.2

Imagined Histories

Imagined Histories

On Far-infrared and Submillimeter Circular Polarization

Abstract Interstellar dust grains are often aligned. If the grain alignment direction varies along the line of sight, the thermal emission becomes circularly polarized. In the diffuse interstellar medium, the circular polarization at far-infrared and submillimeter wavelengths is predicted to be very small, and probably unmeasurable. However, circular polarization may reach detectable levels in photodissociation regions viewed through molecular clouds, in infrared dark clouds, and in protoplanetary disks. Measurement of circular polarization could help constrain the structure of the magnetic field in infrared dark clouds, and may shed light on the mechanisms responsible for grain alignment in protoplanetary disks.

Cloud motion and magnetic fields: Four clouds in the Cepheus Flare region

Context. The Cepheus Flare region consists of a group of dark cloud complexes that are currently active in star formation. Aims. The aim of this work is to estimate the motions of four clouds, namely L1147/1158, L1172/1174, L1228, and L1251, located at relatively high Galactic latitude (b > 14°) in the Cepheus Flare region. We study the relationship between the motions of the clouds with respect to the magnetic field and the clump orientations with respect to both the magnetic field and the motion. Methods. We estimated the motions of the molecular clouds using the proper motion and distance estimates of the young stellar objects (YSOs) associated with them using the Gaia EDR3 data. By assuming that the YSOs are associated with the clouds and share the same velocity, the projected directions of motion are estimated for the clouds. We measured the projected geometry of the magnetic field towards the direction of each cloud by combining the Planck polarization measurements. Results. We estimated a distance of 371 ± 22 pc for L1228 and 340 ± 7 pc for L1251, implying that all four complexes are located at almost the same distance. Assuming that both the clouds and YSOs are kinematically coupled, we estimated the projected direction of motion of the clouds using the proper motions of the YSOs. The directions of motion of all the clouds are offset by ~30° with respect to the ambient magnetic fields, except in L1172/1174 where the offset is ~45°. In L1147/1158, the starless clumps are found to be oriented predominantly parallel to the magnetic fields while prestellar clumps show a random distribution. In L1172/1174, L1228, and L1251, the clumps are oriented randomly with respect to the magnetic field. With respect to the motion of the clouds, there is a marginal trend that the starless clumps are oriented more parallel in L1147/1158 and L1172/1174. In L1228, the major axes of the clumps are oriented more randomly. In L1251, we find a bimodal trend in the case of starless clumps. We do not find any overall specific correlation between the core orientation and the global/local magnetic fields for the clouds in Cepheus. Also, we conclude that the local small-scale dynamics of the cloud with respect to the magnetic field direction could be responsible for the final orientation of the cores.

Observations of multiple NH3 transitions in W33

At a distance of 2.4 kpc, W33 is an outstanding massive and luminous 10 pc-sized star forming complex containing quiescent infrared dark clouds as well as highly active infrared bright cloud cores heated by young massive stars. We report measurements of ammonia (NH3) inversion lines in the frequency range 18–26 GHz obtained with the 40′′ resolution of the 100 m Effelsberg telescope. We detect the (J, K) = (1,1), (2,2), (3,3), (4,4), (5,5), (6,6), (2,1), and (3,2) transitions. There is a maser line in the (3,3) transition towards W33 Main. Brightness temperature and line shape indicate no significant variation during the last ~36 yr. We determined kinetic temperatures, column densities, and other physical properties of NH3 and the molecular clouds in W33. For the total-NH3 column density inside 40′′ (0.5 pc) regions, we find 6.0 (±2.1) × 1014, 3.5 (±0.1) × 1015, 3.4 (±0.2) × 1015, 3.1 (±0.2) × 1015, 2.8 (±0.2) × 1015, and 2.0 (±0.2) × 1015 cm−2 at the peak positions of W33 Main, W33 A, W33 B, W33 Main1, W33 A1, and W33 B1, respectively. W33 Main has a total-NH3 fractional abundance of 1.3 (±0.1) × 10−9 at the peak position. High values of 1.4 (±0.3) × 10−8, 1.6 (±0.3) × 10−8, 3.4 (±0.5) × 10−8, 1.6 (±0.5) × 10−8, and 4.0 (±1.2) × 10−8 are obtained at the central positions of W33 A, W33 B, W33 Main1, W33 A1, and W33 B1. From this, we confirm the previously proposed variation in the evolutionary stages of the six W33 clumps and find that there is no hot core in the region approaching the extreme conditions encountered in W51-IRS2 or Sgr B2. The ortho-to-para-NH3 abundance ratios suggest that ammonia should have been formed in the gas phase or on dust grain mantles at kinetic temperatures of ≳20 K. We determine kinetic temperatures only using NH3 (1,1) and (2,2), and from this we provide gas volume densities for the six main sources in the W33 region. With our new Tkin values, we find that our volume densities are similar to those estimated by Immer et al. (2014, A&A, 572, A63), suggesting that ammonia beam-filling factors are close to unity.

Contact electrification induced mechanoluminescence

Mechanoluminescence (ML) is a luminescence response to mechanical stimuli that shows a variety of significant applications. It is generally believed that ML is due to piezoluminescence in asymmetric piezoelectric materials, but this model encounters difficulties in explaining the ML for centrosymmetric nonpiezoelectric materials, especially the Lu3Al5O12: Ce3+/PDMS elastomer with ultrastrong nonpreirradiation ML. This theoretical problem has become the prominent “dark cloud” in the sky of the ML field. This work reveals for the first time that the ML for the centrosymmetric Lu3Al5O12: Ce3+/PDMS elastomer is essentially induced by contact electrification. According to contact electrification, an electron-cloud model of contact electrification is successfully established to understand the ML mechanism for the elastomer. This demonstrates that contact electrification arising from the interaction of two dissimilar surfaces creates a broadband excitation energy, which directly excites the luminescence levels to emit ML. Accordingly, the unique ML properties of the centrosymmetric Lu3Al5O12: Ce3+/PDMS elastomer that cannot be explained by piezoelectricity can be well understood by contact electrification. Particularly, these results also inspire us to have reasonable new insight into the trap-dependent piezoluminescence mechanism for typical SrAl2O4: Eu2+ and ZnS: Cu/Mn2+ materials.

When would the dark clouds of financial inclusion be over, and the environment becomes clean? The role of national governance.

On one side, the rapid progress in financial development boosts economic growth. On the other hand, it forces both the developed and emerging countries to play the role of good governance that help save the environment. The current study aims to identify the role of national governance in the relationship between financial inclusion and ecological footprints. To attain the study's objective, we use a novel method of moments quantile regression (MMQR) on a panel data set of 65 countries from 2004 to 2017. The empirical outcomes reveal that financial inclusion has a significant positive and heterogeneous impact on ecological footprints. This effect varies across quantiles, and when moving from lower to upper quantiles, the impact of financial inclusion on environmentescalates. National governance plays an important role to moderate the relationship between financial inclusion and ecological footprint negatively. Moreover, GDP and REC display a significant positive and negative influence on ecological footprints, respectively. We obtain similar and robust findings from the alternative panel estimation techniques, including FMOLS, FEOLS, and DOLS. The policy implications from this research can be considered to achieve sustainable and eco-friendly environmental goals.

The silver lining behind the dark cloud: Exploring the psycho-social factors impacting successful adaptation during the COVID-19 pandemic

While most studies have been reporting the psychological issues being faced by the public due to the global spread of coronavirus and sudden restrictions and changes accompanying it, the present study attempted to explore dynamic human experiences during the COVID-19 pandemic and resultant lockdown, so as to understand the psycho-social factors that acted as adaptive resources or as buffers to maintain a stable mental state amidst this crisis. In-depth telephonic interviews with 30 participants were conducted to explore their experiences in dealing with the COVID-19 pandemic and the lockdown. Thematic analysis performed to identify the positive and protective factors that helped people adapt in a healthy way revealed that although the initial response of the participants to the pandemic was “optimistic bias” followed by downplaying the seriousness of the issue, later they demonstrated increased realization and acceptance to the seriousness of the situation. Upon realizing the situation, their positive psychological resources acted as a buffer against the ill effects of the pandemic, and they used both cognitive and behavioral coping. The study clearly demonstrates that crisis in life is not just a source of stress, anxiety, and uncertainty but also an opportunity to test one’s psychological resources to learn and grow.

A complete 3mm line survey of the B1-b and TMC-1 cores

We present the 3mm spectral line survey performed at the IRAM 30m telescope towards the dense cores B1-b and TMC-1. Within the 46 GHz observed, we have identified more than 500 lines arising from more than 60 molecules. We have also detected tens of unidentified lines, allowing the discovery of new molecular species in space. In this contribution we discuss two examples: the case of H2NC and CH3CO+. In the latter, the 30m data was used in combination with the 7mm survey data from the Yebes 40m telescope, which provides lower energy transitions. Our deep 3mm and 7mm spectral surveys reveal a forest of lines at 50-100 mK, showing that dark clouds cannot be considered poor line sources anymore.

Hydrogenation of Accreting C Atoms and CO Molecules–Simulating Ketene and Acetaldehyde Formation Under Dark and Translucent Cloud Conditions

Abstract Simple and complex organic molecules (COMs) are observed along different phases of star and planet formation and have been successfully identified in prestellar environments such as dark and translucent clouds. Yet the picture of organic molecule formation at those earliest stages of star formation is not complete and an important reason is the lack of specific laboratory experiments that simulate carbon atom addition reactions on icy surfaces of interstellar grains. Here we present experiments in which CO molecules as well as C and H atoms are codeposited with H2O molecules on a 10 K surface mimicking the ongoing formation of an “H2O-rich” ice mantle. To simulate the effect of impacting C atoms and resulting surface reactions with ice components, a specialized C-atom beam source is used, implemented on SURFRESIDE3, an ultra-high vacuum cryogenic setup. Formation of ketene (CH2CO) in the solid state is observed in situ by means of reflection absorption IR spectroscopy. C18O and D isotope labeled experiments are performed to further validate the formation of ketene. Data analysis supports that CH2CO is formed through C-atom addition to a CO molecule, followed by successive hydrogenation transferring the formed :CCO into ketene. Efficient formation of ketene is in line with the absence of an activation barrier in C+CO reaction reported in the literature. We also discuss and provide experimental evidence for the formation of acetaldehyde (CH3CHO) and possible formation of ethanol (CH3CH2OH), two COM derivatives of CH2CO hydrogenation. The underlying reaction network is presented and the astrochemical implications of the derived pathways are discussed.

Discovery of the elusive thioketenylium, HCCS+, in TMC-1

We report the detection in TMC-1 of the cation HCCS+ (X̃ 3Σ−), which is the protonated form of the widespread radical CCS. This is the first time that a protonated radical has been detected in a cold dark cloud. Twenty-six hyperfine components from twelve rotational transitions have been observed with the Yebes 40 m and IRAM 30m radio telescopes. We confidently assign the characteristic rotational spectrum pattern to HCCS+ based on the good agreement between the astronomical and theoretical spectroscopic parameters. The column density of HCCS+ is (1.1 ± 0.1)×1012 cm−2, and the CCS/HCCS+ abundance ratio is 50 ± 10, which is very similar to that of CS/HCS+ (35 ± 8) and CCCS/HCCCS+ (65 ± 20). From a state-of-the-art gas-phase chemical model, we conclude that HCCS+ is mostly formed by reactions of proton transfer from abundant cations such as HCO+, H3O+, and H3+ to the radical CCS.

Formation of the acenaphthylene cation as a common C2H2-loss fragment in dissociative ionization of the PAH isomers anthracene and phenanthrene.

Polycyclic aromatic hydrocarbons (PAHs) are thought to be a major constituent of astrophysical environments, being the carriers of the ubiquitous aromatic infrared bands (AIBs) observed in the spectra of galactic and extra-galactic sources that are irradiated by ultraviolet (UV) photons. Small (2-cycles) PAHs were unambiguously detected in the TMC-1 dark cloud, showing that PAH growth pathways exist even at low temperatures. The processing of PAHs by UV photons also leads to their fragmentation, which has been recognized in recent years as an alternative route to the generally accepted bottom-up chemical pathways for the formation of complex hydrocarbons in UV-rich interstellar regions. Here we consider the C12H8+ ion that is formed in our experiments from the dissociative ionization of the anthracene and phenanthrene (C14H10) molecules. By employing the sensitive action spectroscopic scheme of infrared pre-dissociation (IRPD) in a cryogenic ion trap instrument coupled to the free-electron lasers at the FELIX Laboratory, we have recorded the broadband and narrow line-width gas-phase IR spectra of the fragment ions (C12H8+) and also the reference spectra of three low energy isomers of C12H8+. By comparing the experimental spectra to those obtained from quantum chemical calculations we have identified the dominant structure of the fragment ion formed in the dissociation process to be the acenaphthylene cation for both isomeric precursors. Ab initio molecular dynamics simulations are presented to elucidate the fragmentation process. This result reinforces the dominant role of species containing a pentagonal ring in the photochemistry of small PAHs.

Detection of the propargyl radical at λ 3 mm

We report the detection of the propargyl radical (CH2CCH) in the cold dark cloud TMC-1 in the λ 3 mm wavelength band. We recently discovered this species in space toward the same source at a wavelength of λ 8 mm. In those observations, various hyperfine components of the 20,2–10,1 rotational transition, at 37.5 GHz, were detected using the Yebes 40 m telescope. Here, we used the IRAM 30 m telescope to detect ten hyperfine components of the 50,5–40,4 rotational transition, lying at 93.6 GHz. The observed frequencies differ by 0.2 MHz with respect to the predictions from available laboratory data. This difference is significant for a radio-astronomical search for CH2CCH in interstellar sources with narrow lines. We thus included the measured frequencies in a new spectroscopic analysis to provide accurate frequency predictions for the interstellar search for propargyl at millimeter wavelengths. Moreover, we recommend that future searches for CH2CCH in cold interstellar clouds be carried out at λ 3 mm rather than at λ 8 mm. The 50,5–40,4 transition is about five times more intense than the 20,2–10,1 one in TMC-1, which implies that detecting the former requires about seven times less telescope time than detecting the latter. We constrain the rotational temperature of CH2CCH in TMC-1 to 9.9 ± 1.5 K, which indicates that the rotational levels of this species are thermalized at the gas kinetic temperature. The revised value of the column density of CH2CCH (including ortho and para species) is (1.0 ± 0.2) × 1014 cm−2, and thus the CH2CCH/CH3CCH abundance ratio is revised slightly higher, approaching one. This study opens the door to future detections of CH2CCH in other cold interstellar clouds, making it possible to further investigate the role of this very abundant hydrocarbon radical in the synthesis of large organic molecules, such as aromatic rings.

Economic Impact of Mongolia’s Cashmere Export

This paper examines the economic impact of exporting Cashmere by considering every aspect of the product’s performance in the global market and the financial outcomes. The article begins by appraising the cashmere industry’s development and the transition into the global export market. This objective is achieved through a comparative analysis of cashmere export and other country’s economic activities like livestock farming. The contribution of cashmere export to the country’s GDP is cited as a significant economic impact. The exporting of the commodity is the third-largest earner for the country after gold and copper. This indicates the economic significance of exporting Cashmere. The paper is based on primary research from distinct participants through questionnaires and interviews, and analysis to interpret the research findings. The article discusses the evolution of the cashmere industry by examining government support and the growing demand for the products as the factors that led to the emergence of the cashmere economy. This casts a dark cloud over the sustainability of the many economic gains of exporting Cashmere. The paper suggests developing a sound policy framework and creating institutional frameworks to enhance the competitiveness of the cashmere industry, hence guaranteeing the sustainability of the positive economic impact accrued.

Finding the Silver Lining of Opportunities through the Dark Clouds of COVID-19 Pandemic

No single event so far has stumped the world more significantly than the present COVID-19 pandemic. However, every adversity brings with it an opportunity and as medical community, we must evolve in order to survive this unique challenge. This essay throws light on the various opportunities we can seize or have done so in the pandemic. We explore the opportunities in medical education and training, health research, clinical practices and frontline work, public health and awareness, and revenue generation and allocation of resources. Thus, through this article we understand that, “In every adversity lies an opportunity”, an age-old adage has never been truer than in the scenario of the current COVID-19 pandemic.

Gas Dynamics in the Star-forming Region G18.148–0.283: Is It a Manifestation of Two Colliding Molecular Clouds?

Abstract We report the results obtained from a multiwavelength study of the H ii region G18.148−0.283 using the upgraded Giant Metrewave Radio Telescope at 1350 MHz, along with other archival data. In addition to the radio continuum emission, we have detected the H169α and H170α radio recombination lines toward G18.148−0.283 using a correlator bandwidth of 100 MHz. The moment-1 map of the ionized gas reveals a velocity gradient of approximately 10 km s−1 across the radio continuum peaks. The 12CO (J = 3−2) molecular line data from the CO High-Resolution Survey (COHRS) also show the presence of two velocity components that are very close to the velocities detected in the ionized gas. The spectrum and position–velocity diagram from CO emission reveal molecular gas at an intermediate-velocity range bridging the velocity components. We see mid-infrared absorption and far-infrared emission establishing the presence of a filamentary infrared dark cloud, the extent of which includes the targeted H ii region. The magnetic field inferred from dust polarization is perpendicular to the filament within the H ii region. We have also identified two O9 stars and 30 young stellar objects toward the target using data from the Two Micron All Sky Survey (2MASS), UKIRT Infrared Deep Sky Survey (UKIDSS), and Galactic Legacy Infrared Midplane Survey Extraordinaire (GLIMPSE). Cumulatively, this suggests that the region is the site of a cloud–cloud collision that has triggered massive star formation and subsequent formation of an H ii region.

Deep Learning Framework for Precipitation Prediction Using Cloud Images

Precipitation prediction (PP) have become one of the significant research areas of deep learning (DL) and machine vision (MV) techniques are frequently used to predict the weather variables (WV). Since the climate change has left significant impact upon weather variables (WV) and continuously changes are observed in temperature, humidity, cloud patterns and other factors. Although cloud images contain sufficient information to predict the precipitation pattern but due to changes in climate, the complex cloud patterns and rapid shape changing behavior of clouds are difficult to consider for rainfall prediction. Prediction of rainfall would provide more meticulous assistance to the farmers to know about the weather conditions and to care their cash crops. This research proposes a framework to classify the dark cloud patterns (DCP) for prediction of precipitation. The framework consists upon three steps to classify the cloud images, first step tackles noise reduction operations, feature selection and preparation of datasets. Second step construct the decision model by using convolutional neural network (CNN) and third step presents the performance visualization by using confusion matrix, precision, recall and accuracy measures. This research contributes (1) real-world clouds datasets (2) method to prepare datasets (3) highest classification accuracy to predict estimated as 96.90%.

Mechanisms for gas-phase molecular formation of neutral formaldehyde (H2CO) in cold astrophysical regions

Context. Formaldehyde is a potential biogenic precursor involved in prebiotic chemical evolution. The cold conditions of the interstellar medium (ISM) allow H2CO to be reactive, playing a significant role as a chemical intermediate in formation pathways leading to interstellar complex organic molecules. However, gas-phase molecular formation mechanisms in cold regions of the ISM are poorly understood. Aims. We computationally determine the most favored gas-phase molecular formation mechanisms at local thermodynamic equilibrium conditions that can produce the detected amounts of H2CO in diffuse molecular clouds (DMCs), in dark, cold, and dense molecular clouds (DCDMCs), and in three regions of circumstellar envelopes of low-mass protostars (CELMPs). Methods. The potential energy surfaces, thermodynamic functions, and single-point energies for transition states were calculated at the CCSD(T)-F12/cc-pVTZ-F12 and MP2/aug-cc-pVDZ levels of theory and basis sets. Molecular thermodynamics and related partition functions were obtained by applying the Maxwell-Boltzmann quantum statistics theory from energies computed at CCSD(T)-F12/cc-pVTZ-F12 with corrections for zero-point energy. A literature review on detected abundances of reactants helped us to propose the most favorable formation routes. Results. The most probable reactions that produce H2CO in cold astrophysical regions are: 1CH2 + ⋅3O2 →1H2CO + O⋅(3P) in DMCs, ⋅3CH2 + ⋅3O2 →1H2CO + ⋅O(3P) in DCDMCs, and ⋅CH3 + ⋅O(3P) →1H2CO + ⋅H in region III, ⋅CH3 +⋅O(1D) →1H2CO + ⋅H in region II, and 1CH2 + ⋅3O2 →1H2CO + ⋅O(3P) in region I belonging to CELMPs. Conclusions. Quantum chemical calculations suggest that the principal carbonaceous precursors of H2CO in cold regions for the gas-phase are CH2(a1A1), and ⋅CH2(X3B1) combined with ⋅O2(3Σg) and ⋅CH3(2A”) + ⋅O(3P) / O(1D). Reactions based on more complex reagents yield less effective thermodynamics in the gas-phase H2CO molecular formation.

The Rise and Gradual Decline of Israeli Democracy, 1920–2020

The article discusses the developmental stages of Israeli democracy: from the pre-state Jewish Yishuv, to the formative years of democracy in Israel; from the 1950s to the early 1960s; and during the years of liberalization and democratization, from the mid-1960s until the early 1980s. However, since the 1980s, the sense of inclusiveness and equality in Israeli society has gradually declined, amid antidemocratic legislation and the spread of antidemocratic incitement, polarization and authoritarian challenges to the political system. The article observes the dark clouds that threaten Israel's democracy and the struggle between its democratic and antidemocratic forces.

The ALMA Survey of 70 μm Dark High-mass Clumps in Early Stages (ASHES). IV. Star Formation Signatures in G023.477

Abstract With a mass of ∼1000 M ⊙ and a surface density of ∼0.5 g cm−2, G023.477+0.114, also known as IRDC 18310-4, is an infrared dark cloud (IRDC) that has the potential to form high-mass stars and has been recognized as a promising prestellar clump candidate. To characterize the early stages of high-mass star formation, we have observed G023.477+0.114 as part of the Atacama Large Millimeter/submillimeter Array (ALMA) Survey of 70 μm Dark High-mass Clumps in Early Stages. We have conducted ∼1.″2 resolution observations with ALMA at 1.3 mm in dust continuum and molecular line emission. We have identified 11 cores, whose masses range from 1.1 to 19.0 M ⊙. Ignoring magnetic fields, the virial parameters of the cores are below unity, implying that the cores are gravitationally bound. However, when magnetic fields are included, the prestellar cores are close to virial equilibrium, while the protostellar cores remain sub-virialized. Star formation activity has already started in this clump. Four collimated outflows are detected in CO and SiO. H2CO and CH3OH emission coincide with the high-velocity components seen in the CO and SiO emission. The outflows are randomly oriented for the natal filament and the magnetic field. The position-velocity diagrams suggest that episodic mass ejection has already begun even in this very early phase of protostellar formation. The masses of the identified cores are comparable to the expected maximum stellar mass that this IRDC could form (8–19 M ⊙). We explore two possibilities on how IRDC G023.477+0.114 could eventually form high-mass stars in the context of theoretical scenarios.