7,058 results on '"Jordan, C."'
Search Results
2. JWST view of four infant galaxies at z=8.31-8.49 in the MACS0416 field and implications for reionization
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Ma, Zhiyuan, Sun, Bangzheng, Cheng, Cheng, Yan, Haojing, Sun, Fengwu, Foo, Nicholas, Egami, Eiichi, Diego, Jose M., Cohen, Seth H., Jansen, Rolf A., Summers, Jake, Windhorst, Rogier A., D'Silva, Jordan C. J., Koekemoer, Anton M., Coe, Dan, Conselice, Christopher J., Driver, Simon P., Frye, Brenda, Grogin, Norman A., Marshall, Madeline A., Nonino, Mario, Ortiz III, Rafael, Pirzkal, Nor, Robotham, Aaron, Ryan, Jr., Russell E., Willmer, Christopher N. A., Adams, Nathan J., Hathi, Nimish P., Dole, Herve, Willner, S. P., Espada, Daniel, Furtak, Lukas J., Hsiao, Tiger Yu-Yang, Li, Qiong, Chen, Wenlei, Jolly, Jean-Baptiste, and Chen, Chian-Chou
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Astrophysics - Astrophysics of Galaxies - Abstract
New JWST/NIRCam wide-field slitless spectroscopy provides redshifts for four z>8 galaxies located behind the lensing cluster MACS J0416.1-2403. Two of them, "Y1" and "JD", have previously reported spectroscopic redshifts based on ALMA measurements of [OIII] 88 $\mu$m and/or [CII] 157.7 $\mu$m lines. Y1 is a merging system of three components, and the existing redshift z=8.31 is confirmed. However, JD is at z=8.34 instead of the previously claimed z=9.28. JD's close companion, "JD-N", which was a previously discovered z>8 candidate, is now identified at the same redshift as JD. JD and JD-N form an interacting pair. A new candidate at z>8, "f090d_018", is also confirmed and is at z=8.49. These four objects are likely part of an overdensity that signposts a large structure extending ~165 kpc in projected distance and ~48.7 Mpc in radial distance. They are magnified by less than one magnitude and have intrinsic $M_{UV}$ ranging from -19.57 to -20.83 mag. Their spectral energy distributions show that the galaxies are all very young with ages ~ 4-18 Myr and stellar masses about $10^{7-8}$ ${\rm M_\odot}$. These infant galaxies have very different star formation rates ranging from a few to over a hundred $\rm{M_\odot}$ yr$^{-1}$, but only two of them (JD and f090d_018) have blue rest-frame UV slopes $\beta<-2.0$ indicative of a high Lyman-continuum photon escape fraction that could contribute significantly to the cosmic hydrogen-reionizing background. Interestingly, these two galaxies are the least massive and least active ones among the four. The other two systems have much flatter UV slopes largely because of their high dust extinction ($A_{\rm V}$=0.9-1.0 mag). Their much lower indicated escape fractions show that even very young, actively star-forming galaxies can have negligible contribution to reionization when they quickly form dust throughout their bodies., Comment: 18 pages, 6 figures, after addressing the referee report
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- 2024
3. Selecting focused digital cohorts from social media using the metric backbone of biomedical knowledge graphs
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Guo, Ziqi, Felag, Jack, Rozum, Jordan C., Correia, Rion Brattig, and Rocha, Luis M.
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Computer Science - Social and Information Networks - Abstract
The abundance of social media data allows researchers to construct large digital cohorts to study the interplay between human behavior and medical treatment. Identifying the users most relevant to a specific health problem is, however, a challenge in that social media sites vary in the generality of their discourse. While X (formerly Twitter), Instagram, and Facebook cater to wide ranging topics, Reddit subgroups and dedicated patient advocacy forums trade in much more specific, biomedically-relevant discourse. To hone in on relevant users anywhere, we have developed a general framework and applied it to epilepsy discourse in social media as a test case. We analyzed the text from posts by users who mention epilepsy drugs in the general-purpose social media sites X and Instagram, the epilepsy-focused Reddit subgroup (r/Epilepsy), and the Epilepsy Foundation of America (EFA) forums. We curated a medical terms dictionary and used it to generate a knowledge graph (KG) for each online community. For each KG, we computed the metric backbone--the smallest subgraph that preserves all shortest paths in the network. By comparing the subset of users who contribute to the backbone to the subset who do not, we found that epilepsy-focused social media users contribute to the KG backbone in much higher proportion than do general-purpose social media users. Furthermore, using human annotation of Instagram posts, we demonstrated that users who do not contribute to the backbone are more than twice as likely to use dictionary terms in a manner inconsistent with their biomedical meaning. For biomedical research applications, our backbone-based approach thus has several benefits over simple engagement-based approaches: It can retain low-engagement users who nonetheless contribute meaningful biomedical insights. It can filter out very vocal users who contribute no relevant content.
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- 2024
4. myAURA: Personalized health library for epilepsy management via knowledge graph sparsification and visualization
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Correia, Rion Brattig, Rozum, Jordan C., Cross, Leonard, Felag, Jack, Gallant, Michael, Guo, Ziqi, Herr II, Bruce W., Min, Aehong, Rocha, Deborah Stungis, Wang, Xuan, Börner, Katy, Miller, Wendy, and Rocha, Luis M.
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Computer Science - Information Retrieval ,Computer Science - Digital Libraries - Abstract
Objective: We report the development of the patient-centered myAURA application and suite of methods designed to aid epilepsy patients, caregivers, and researchers in making decisions about care and self-management. Materials and Methods: myAURA rests on the federation of an unprecedented collection of heterogeneous data resources relevant to epilepsy, such as biomedical databases, social media, and electronic health records. A generalizable, open-source methodology was developed to compute a multi-layer knowledge graph linking all this heterogeneous data via the terms of a human-centered biomedical dictionary. Results: The power of the approach is first exemplified in the study of the drug-drug interaction phenomenon. Furthermore, we employ a novel network sparsification methodology using the metric backbone of weighted graphs, which reveals the most important edges for inference, recommendation, and visualization, such as pharmacology factors patients discuss on social media. The network sparsification approach also allows us to extract focused digital cohorts from social media whose discourse is more relevant to epilepsy or other biomedical problems. Finally, we present our patient-centered design and pilot-testing of myAURA, including its user interface, based on focus groups and other stakeholder input. Discussion: The ability to search and explore myAURA's heterogeneous data sources via a sparsified multi-layer knowledge graph, as well as the combination of those layers in a single map, are useful features for integrating relevant information for epilepsy. Conclusion: Our stakeholder-driven, scalable approach to integrate traditional and non-traditional data sources, enables biomedical discovery and data-powered patient self-management in epilepsy, and is generalizable to other chronic conditions.
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- 2024
5. EPOCHS III: Unbiased UV continuum slopes at 6.5<z<13 from combined PEARLS GTO and public JWST NIRCam imaging
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Austin, Duncan, Conselice, Christopher J., Adams, Nathan J., Harvey, Thomas, Duan, Qiao, Trussler, James, Li, Qiong, Juodzbalis, Ignas, Ormerod, Katherine, Ferreira, Leonardo, Westcott, Lewi, Harris, Honor, Wilkins, Stephen M., Bhatawdekar, Rachana, Caruana, Joseph, Coe, Dan, Cohen, Seth H., Driver, Simon P., D'Silva, Jordan C. J., Frye, Brenda, Furtak, Lukas J., Grogin, Norman A., Hathi, Nimish P., Holwerda, Benne W., Jansen, Rolf A., Koekemoer, Anton M., Marshall, Madeline A., Nonino, Mario, Ortiz III, Rafael, Pirzkal, Nor, Robotham, Aaron, Ryan Jr., Russell E., Summers, Jake, Willmer, Christopher N. A., Windhorst, Rogier A., Yan, Haojing, and Zackrisson, Erik
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Astrophysics - Astrophysics of Galaxies - Abstract
We present an analysis of rest-frame UV continuum slopes, $\beta$, using a sample of 1011 galaxies at $6.5
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- 2024
6. PEARLS: Discovery of Point-Source Features Within Galaxies in the North Ecliptic Pole Time Domain Field
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Ortiz III, Rafael, Windhorst, Rogier A., Cohen, Seth H., Willner, S. P., Jansen, Rolf A., Carleton, Timothy, Kamieneski, Patrick S., Rutkowski, Michael J., Smith, Brent, Summers, Jake, McCabe, Tyler J., O'Brien, Rosalia, Diego, Jose M., Yun, Min S., D'Silva, Jordan C. J., Li, Juno, Gim, Hansung B., Hathi, Nimish P., Holwerda, Benne W., Zitrin, Adi, Cheng, Cheng, McLeod, Noah J., Conselice, Christopher J., Driver, Simon P., Yan, Haojing, Coe, Dan, Frye, Brenda, Grogin, Norman, Koekemoer, Anton, Marshall, Madeline A., Pirzkal, Nor, Robotham, Aaron, Ryan, Jr., Russell E., Willmer, Christopher N. A., Keel, William, Hammel, H. B., Hyun, M., Im, M., and Milam, S. N.
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Astrophysics - Astrophysics of Galaxies - Abstract
The first public 0.9-4.4{\mu}m NIRCam images of the North Ecliptic Pole (NEP) Time Domain Field (TDF) uncovered galaxies displaying point-source features in their cores as seen in the longer wavelength filters. We visually identified a sample of 66 galaxies (~1 galaxy per arcmin2) with point-like cores and have modeled their two-dimensional light profiles with GalFit, identifying 16 galactic nuclei with measurable point-source components. GalFit suggests the visual sample is a mix of both compact stellar bulge and point-source galaxy cores. This core classification is complemented by spectral energy distribution (SED) modeling to infer the sample's active galactic nucleus (AGN) and host-galaxy parameters. For galaxies with measurable point-source components, the median fractional AGN contribution to their 0.1-30.0{\mu}m flux is 0.44, and 14/16 are color-classified AGN. We conclude that near-infrared point-source galaxy cores are signatures of AGN. In addition, we define an automated sample-selection criterion to identify these point-source features. These criteria can be used in other extant and future NIRCam images to streamline the search for galaxies with unresolved IR-luminous AGN. The James Webb Space Telescope's superb angular resolution and sensitivity at infrared wavelengths is resurrecting the morphological identification of AGN., Comment: 17 pages, 9 figures, 2 tables
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- 2024
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7. Birds of a Feather: Resolving Stellar Mass Assembly With JWST/NIRCam in a Pair of Kindred $z \sim 2$ Dusty Star-forming Galaxies Lensed by the PLCK G165.7+67.0 Cluster
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Kamieneski, Patrick S., Frye, Brenda L., Windhorst, Rogier A., Harrington, Kevin C., Yun, Min S., Noble, Allison, Pascale, Massimo, Foo, Nicholas, Cohen, Seth H., Jansen, Rolf A., Carleton, Timothy, Koekemoer, Anton M., Willmer, Christopher N. A., Summers, Jake S., Garuda, Nikhil, Leimbach, Reagen, Holwerda, Benne W., Pierel, Justin D. R., Jimenez-Andrade, Eric F., Willner, S. P., Pampliega, Belen Alcalde, Vishwas, Amit, Keel, William C., Wang, Q. Daniel, Cheng, Cheng, Coe, Dan, Conselice, Christopher J., D'Silva, Jordan C. J., Driver, Simon P., Grogin, Norman A., Hinrichs, Tyler, Lowenthal, James D., Marshall, Madeline A., Nonino, Mario, Ortiz III, Rafael, Pigarelli, Alex, Pirzkal, Nor, Polletta, Maria del Carmen, Robotham, Aaron S. G., Ryan Jr., Russell E., and Yan, Haojing
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Astrophysics - Astrophysics of Galaxies - Abstract
We present a new parametric lens model for the G165.7+67.0 galaxy cluster, which was discovered with $Planck$ through its bright submillimeter flux, originating from a pair of extraordinary dusty star-forming galaxies (DSFGs) at $z\approx 2.2$. Using JWST and interferometric mm/radio observations, we characterize the intrinsic physical properties of the DSFGs, which are separated by only $\sim 1^{\prime\prime}$ (8 kpc) and a velocity difference $\Delta V \lesssim 600~{\rm km}~{\rm s}^{-1}$ in the source plane, and thus likely undergoing a major merger. Boasting intrinsic star formation rates ${\rm SFR}_{\rm IR} = 320 \pm 70$ and $400 \pm 80~ M_\odot~{\rm yr}^{-1}$, stellar masses ${\rm log}[M_\star/M_\odot] = 10.2 \pm 0.1$ and $10.3 \pm 0.1$, and dust attenuations $A_V = 1.5 \pm 0.3$ and $1.2 \pm 0.3$, they are remarkably similar objects. We perform spatially-resolved pixel-by-pixel SED fitting using rest-frame near-UV to near-IR imaging from JWST/NIRCam for both galaxies, resolving some stellar structures down to 100 pc scales. Based on their resolved specific SFRs and $UVJ$ colors, both DSFGs are experiencing significant galaxy-scale star formation events. If they are indeed interacting gravitationally, this strong starburst could be the hallmark of gas that has been disrupted by an initial close passage. In contrast, the host galaxy of the recently discovered triply-imaged SN H0pe has a much lower SFR than the DSFGs, and we present evidence for the onset of inside-out quenching and large column densities of dust even in regions of low specific SFR. Based on the intrinsic SFRs of the DSFGs inferred from UV through FIR SED modeling, this pair of objects alone is predicted to yield an observable $1.1 \pm 0.2~{\rm CCSNe~yr}^{-1}$, making this cluster field ripe for continued monitoring., Comment: 47 pages, 21 figures, 5 tables. Submitted to ApJ, comments welcome!
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- 2024
8. Verifying the Australian MWA EoR pipeline I: 21-cm sky model and correlated measurement density
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Line, J. L. B., Trott, C. M., Cook, J. H., Greig, B., Barry, N., and Jordan, C. H.
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Astrophysics - Instrumentation and Methods for Astrophysics ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
We present the first of two papers dedicated to verifying the Australian Epoch of Reionisation pipeline (AusEoRPipe) through simulation. The AusEoRPipe aims to disentangle 21-cm radiation emitted by gas surrounding the very first stars from contaminating foreground astrophysical sources, and has been in development for close to a decade. In this paper, we build an accurate 21-cm sky model that can be used by the WODEN simulation software to create visibilities containing a predictable 21-cm signal. We verify that the power spectrum estimator CHIPS can recover this signal in the absence of foregrounds. We also investigate how measurements in Fourier-space are correlated, and how their gridded density affects the power spectrum. We measure and fit for this effect using Gaussian-noise simulations of the MWA phase I layout. We find a gridding density correction factor of 2.651 appropriate for integrations equal to or greater than 30 minutes of data, which contain observations with multiple primary beam pointings and LSTs. Paper II of this series will use the results of this paper to test the AusEoRPipe in the presence of foregrounds and instrumental effects., Comment: 13 pages, 11 Figures, 1 table, accepted in the Publications of the Astronomical Society of Australia (PASA)
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- 2024
9. Single-stranded pre-methylated 5mC adapters uncover the methylation profile of plasma ultrashort Single-stranded cell-free DNA
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Cheng, Jordan C, Swarup, Neeti, Morselli, Marco, Huang, Wei-Lun, Aziz, Mohammad, Caggiano, Christa, Kordi, Misagh, Patel, Abhijit A, Chia, David, Kim, Yong, Li, Feng, Wei, Fang, Zaitlen, Noah, Krysan, Kostyantyn, Dubinett, Steve, Pellegrini, Matteo, and Wong, David TW
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Biological Sciences ,Bioinformatics and Computational Biology ,Genetics ,Cancer Genomics ,Human Genome ,Cancer ,Genetic Testing ,DNA Methylation ,Humans ,Cell-Free Nucleic Acids ,CpG Islands ,DNA ,Single-Stranded ,5-Methylcytosine ,Lung Neoplasms ,Sulfites ,Promoter Regions ,Genetic ,Sequence Analysis ,DNA ,Whole Genome Sequencing ,Environmental Sciences ,Information and Computing Sciences ,Developmental Biology ,Biological sciences ,Chemical sciences ,Environmental sciences - Abstract
Whole-genome bisulfite sequencing (BS-Seq) measures cytosine methylation changes at single-base resolution and can be used to profile cell-free DNA (cfDNA). In plasma, ultrashort single-stranded cfDNA (uscfDNA, ∼50 nt) has been identified together with 167 bp double-stranded mononucleosomal cell-free DNA (mncfDNA). However, the methylation profile of uscfDNA has not been described. Conventional BS-Seq workflows may not be helpful because bisulfite conversion degrades larger DNA into smaller fragments, leading to erroneous categorization as uscfDNA. We describe the '5mCAdpBS-Seq' workflow in which pre-methylated 5mC (5-methylcytosine) single-stranded adapters are ligated to heat-denatured cfDNA before bisulfite conversion. This method retains only DNA fragments that are unaltered by bisulfite treatment, resulting in less biased uscfDNA methylation analysis. Using 5mCAdpBS-Seq, uscfDNA had lower levels of DNA methylation (∼15%) compared to mncfDNA and was enriched in promoters and CpG islands. Hypomethylated uscfDNA fragments were enriched in upstream transcription start sites (TSSs), and the intensity of enrichment was correlated with expressed genes of hemopoietic cells. Using tissue-of-origin deconvolution, we inferred that uscfDNA is derived primarily from eosinophils, neutrophils, and monocytes. As proof-of-principle, we show that characteristics of the methylation profile of uscfDNA can distinguish non-small cell lung carcinoma from non-cancer samples. The 5mCAdpBS-Seq workflow is recommended for any cfDNA methylation-based investigations.
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- 2024
10. The ultrametric backbone is the union of all minimum spanning forests
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Rozum, Jordan C and Rocha, Luis M
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Computer Science - Discrete Mathematics - Abstract
Minimum spanning trees and forests are powerful sparsification techniques that remove cycles from weighted graphs to minimize total edge weight while preserving node connectivity. They have applications in computer science, network science, and graph theory. Despite their utility and ubiquity, they have several limitations, including that they are only defined for undirected networks, they significantly alter dynamics on networks, and they do not generally preserve important network features such as shortest distances, shortest path distribution, and community structure. In contrast, distance backbones, which are subgraphs formed by all edges that obey a generalized triangle inequality, are well defined in both directed and undirected graphs and preserve those and other important network features. The backbone of a graph is defined with respect to a specified path-length operator that aggregates weights along a path to define its length, thereby associating a cost to indirect connections. The backbone is the union of all shortest paths between each pair of nodes according to the specified operator. One such operator, the max function, computes the length of a path as the largest weight of the edges that compose it (a weakest link criterion). It is the only operator that yields an algebraic structure for computing shortest paths that is consistent with De Morgan's laws. Applying this operator yields the ultrametric backbone of a graph in that (semi-triangular) edges whose weights are larger than the length of an indirect path connecting the same nodes (i.e., those that break the generalized triangle inequality based on max as a path-length operator) are removed. We show that the ultrametric backbone is the union of all minimum spanning forests in undirected graphs and provides a new generalization of minimum spanning trees to directed graphs., Comment: 10 pages, 1 figure. Revision corrects typo in abstract
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- 2024
11. The Efficacy of Telemental Health Interventions for Mood Disorders Pre-COVID-19: A Narrative Review
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Edwards, Alyssa M., Petitt, Jordan C., Sajatovic, Martha, Kumar, Sanjana, and Levin, Jennifer B.
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- 2024
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12. A review on the impact of single-stranded library preparation on plasma cell-free diversity for cancer detection
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Cheng, Jordan C, Swarup, Neeti, Wong, David TW, and Chia, David
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Biomedical and Clinical Sciences ,Oncology and Carcinogenesis ,Cancer Genomics ,Genetic Testing ,Cancer ,Genetics ,Prevention ,Human Genome ,cell-free DNA ,liquid biopsy ,single-stranded library preparation ,fragment-size ,ultrashort single-stranded cell-free DNA ,Clinical sciences ,Oncology and carcinogenesis - Abstract
In clinical oncology, cell-free DNA (cfDNA) has shown immense potential in its ability to noninvasively detect cancer at various stages and monitor the progression of therapy. Despite the rapid improvements in cfDNA liquid biopsy approaches, achieving the required sensitivity to detect rare tumor-derived cfDNA still remains a challenge. For next-generation sequencing, the perceived presentation of cfDNA is strongly linked to the extraction and library preparation protocols. Conventional double-stranded DNA library preparation (dsDNA-LP) focuses on assessing ~167bp double-stranded mononucleosomal (mncfDNA) and its other oligonucleosomal cell-free DNA counterparts in plasma. However, dsDNA-LP methods fail to include short, single-stranded, or nicked DNA in the final library preparation, biasing the representation of the actual cfDNA populations in plasma. The emergence of single-stranded library preparation (ssDNA-LP) strategies over the past decade has now allowed these other populations of cfDNA to be studied from plasma. With the use of ssDNA-LP, single-stranded, nicked, and ultrashort cfDNA can be comprehensively assessed for its molecular characteristics and clinical potential. In this review, we overview the current literature on applications of ssDNA-LP on plasma cfDNA from a potential cancer liquid biopsy perspective. To this end, we discuss the molecular principles of single-stranded DNA adapter ligation, how library preparation contributes to the understanding of native cfDNA characteristics, and the potential for ssDNA-LP to improve the sensitivity of circulating tumor DNA detection. Additionally, we review the current literature on the newly reported species of plasma ultrashort single-stranded cell-free DNA plasma, which appear biologically distinct from mncfDNA. We conclude with a discussion of future perspectives of ssDNA-LP for liquid biopsy endeavors.
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- 2024
13. JWST's PEARLS: 119 multiply imaged galaxies behind MACS0416, lensing properties of caustic crossing galaxies, and the relation between halo mass and number of globular clusters at $z=0.4$
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Diego, Jose M., Adams, Nathan J., Willner, Steven, Harvey, Tom, Broadhurst, Tom, Cohen, Seth H., Jansen, Rolf A., Summers, Jake, Windhorst, Rogier A., D'Silva, Jordan C. J., Koekemoer, Anton M., Coe, Dan, Conselice, Christopher J., Driver, Simon P., Frye, Brenda, Grogin, Norman A., Marshall, Madeline A., Nonino, Mario, Ortiz III, Rafael, Pirzkal, Nor, Robotham, Aaron, Ryan, Jr., Russell E., Willmer, Christopher N. A., Yan, Haojing, Sun, Fengwu, Hainline, Kevin, Berkheimer, Jessica, Polletta, Maria del Carmen, and Zitrin, Adi
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Astrophysics - Cosmology and Nongalactic Astrophysics ,Astrophysics - Astrophysics of Galaxies - Abstract
We present a new lens model for the $z=0.396$ galaxy cluster MACS J0416.1$-$2403 based on a previously known set of 77 spectroscopically confirmed, multiply imaged galaxies plus an additional set of 42 candidate multiply imaged galaxies from past HST and new JWST data. The new galaxies lack spectroscopic redshifts but have geometric and/or photometric redshift estimates that are presented here. The new model predicts magnifications and time delays for all multiple images. The full set of constraints totals 343, constituting the largest sample of multiple images lensed by a single cluster to date. Caustic-crossing galaxies lensed by this cluster are especially interesting. Some of these galaxies show transient events, most of which are interpreted as micro-lensing of stars at cosmological distances. These caustic-crossing arcs are expected to show similar events in future, deeper JWST observations. We provide time delay and magnification models for all these arcs. The time delays and the magnifications for different arcs are generally anti-correlated, as expected from $N$-body simulations. In the major sub-halos of the cluster, the dark-matter mass from our lens model correlates well with the observed number of globular clusters. This confirms earlier results, derived at lower redshifts, which suggest that globular clusters can be used as powerful mass proxies for the halo masses when lensing constraints are scarce or not available., Comment: 21 pages and 11 figures. Accepted for publication in A&A
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- 2023
14. JWST's PEARLS: Improved Flux Calibration for NIRCam
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Ma, Zhiyuan, Yan, Haojing, Sun, Bangzheng, Cohen, Seth H., Jansen, Rolf A., Summers, Jake, Windhorst, Rogier A., D'Silva, Jordan C. J., Koekemoer, Anton M., Coe, Dan, Conselice, Christopher J., Driver, Simon P., Frye, Brenda, Grogin, Norman A., Marshall, Madeline A., Nonino, Mario, Ortiz III, Rafael, Pirzkal, Nor, Robotham, Aaron, Ryan, Jr., Russell E., Willmer, Christopher N. A., Hammel, Heidi B., Milam, Stefanie N., Adams, Nathan J., Cheng, Cheng, and Hathi, Nimish P.
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Astrophysics - Instrumentation and Methods for Astrophysics - Abstract
The Prime Extragalactic Areas for Reionization and Lensing Science (PEARLS), a JWST GTO program, obtained a set of unique NIRCam observations that have enabled us to significantly improve the default photometric calibration across both NIRCam modules. The observations consisted of three epochs of 4-band (F150W, F200W, F356W, and F444W) NIRCam imaging in the Spitzer IRAC Dark Field (IDF). The three epochs were six months apart and spanned the full duration of Cycle 1. As the IDF is in the JWST continuous viewing zone, we were able to design the observations such that the two modules of NIRCam, modules A and B, were flipped by 180 degrees and completely overlapped each other's footprints in alternate epochs. We were therefore able to directly compare the photometry of the same objects observed with different modules and detectors, and we found significant photometric residuals up to ~ 0.05 mag in some detectors and filters, for the default version of the calibration files that we used (jwst_1039.pmap). Moreover, there are multiplicative gradients present in the data obtained in the two long-wavelength bands. The problem is less severe in the data reduced using the latest pmap (jwst_1130.pmap as of September 2023), but it is still present, and is non-negligible. We provide a recipe to correct for this systematic effect to bring the two modules onto a more consistent calibration, to a photometric precision better than ~ 0.02 mag., Comment: 12 pages, 8 figures, 3 tables. Accepted to PASP
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- 2023
15. Boolean Networks as Predictive Models of Emergent Biological Behaviors
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Rozum, Jordan C., Campbell, Colin, Newby, Eli, Nasrollahi, Fatemeh Sadat Fatemi, and Albert, Reka
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Quantitative Biology - Molecular Networks ,Nonlinear Sciences - Cellular Automata and Lattice Gases - Abstract
Interacting biological systems at all organizational levels display emergent behavior. Modeling these systems is made challenging by the number and variety of biological components and interactions (from molecules in gene regulatory networks to species in ecological networks) and the often-incomplete state of system knowledge (e.g., the unknown values of kinetic parameters for biochemical reactions). Boolean networks have emerged as a powerful tool for modeling these systems. We provide a methodological overview of Boolean network models of biological systems. After a brief introduction, we describe the process of building, analyzing, and validating a Boolean model. We then present the use of the model to make predictions about the system's response to perturbations and about how to control (or at least influence) its behavior. We emphasize the interplay between structural and dynamical properties of Boolean networks and illustrate them in three case studies from disparate levels of biological organization., Comment: Review, to appear in the Cambridge Elements series
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- 2023
16. Evidence of Ultra-faint Radio Frequency Interference in Deep 21~cm Epoch of Reionization Power Spectra with the Murchison Widefield Array
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Wilensky, Michael J., Morales, Miguel F., Hazelton, Bryna J., Star, Pyxie L., Barry, Nichole, Byrne, Ruby, Jordan, C. H., Jacobs, Daniel C., Pober, Jonathan C., and Trott, C. M.
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Astrophysics - Cosmology and Nongalactic Astrophysics ,Astrophysics - Instrumentation and Methods for Astrophysics - Abstract
We present deep upper limits from the 2014 Murchison Widefield Array (MWA) Phase I observing season, with a particular emphasis on identifying the spectral fingerprints of extremely faint radio frequency interference (RFI) contamination in the 21~cm power spectra (PS). After meticulous RFI excision involving a combination of the \textsc{SSINS} RFI flagger and a series of PS-based jackknife tests, our lowest upper limit on the Epoch of Reionization (EoR) 21~cm PS signal is $\Delta^2 \leq 1.61\cdot10^4 \text{ mK}^2$ at $k=0.258\text{ h Mpc}^{-1}$ at a redshift of 7.1 using 14.7 hours of data. By leveraging our understanding of how even fainter RFI is likely to contaminate the EoR PS, we are able to identify ultra-faint RFI signals in the cylindrical PS. Surprisingly this signature is most obvious in PS formed with less than an hour of data, but is potentially subdominant to other systematics in multiple-hour integrations. Since the total RFI budget in a PS detection is quite strict, this nontrivial integration behavior suggests a need to more realistically model coherently integrated ultra-faint RFI in PS measurements so that its potential contribution to a future detection can be diagnosed., Comment: Update acknowledgements, author metadata, and attach journal doi
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- 2023
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17. Star formation and AGN activity 500 Myr after the Big Bang: Insights from JWST
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D'Silva, Jordan C. J., Driver, Simon P., Lagos, Claudia D. P., Robotham, Aaron S. G., Summers, Jake, and Windhorst, Rogier A.
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Astrophysics - Astrophysics of Galaxies - Abstract
We consider the effect of including an active galactic nuclei (AGN) component when fitting spectral energy distributions of 109 spectroscopically confirmed $z\approx 3.5-12.5$ galaxies with JWST. Remarkably, we find that the resulting cosmic star formation history is $\approx 0.4$ dex lower at $z\gtrsim 9.5$ when an AGN component is included in the fitting. This alleviates previously reported excess star formation at $z\gtrsim 9.5$ compared to models based on typical baryon conversion efficiencies inside dark matter halos. We find that the individual stellar masses and star formation rates can be as much as $\approx 4$ dex lower when fitting with an AGN component. These results highlight the importance of considering both stellar mass assembly and supermassive black hole growth when interpreting the light distributions of among the first galaxies to ever exist., Comment: 15 pages, 5 figures. Accepted for publication in ApJL after addressing reviewer comments
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- 2023
18. PEARLS: A Potentially Isolated Quiescent Dwarf Galaxy with a TRGB Distance of 30 Mpc
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Carleton, Timothy, Ellsworth-Bowers, Timothy, Windhorst, Rogier A., Cohen, Seth H., Conselice, Christopher J., Diego, Jose M., Zitrin, Adi, Archer, Haylee N., McIntyre, Isabel, Kamieneski, Patrick, Jansen, Rolf A., Summers, Jake, D'Silva, Jordan C. J., Koekemoer, Anton M., Coe, Dan, Driver, Simon P., Frye, Brenda, Grogin, Norman A., Marshall, Madeline A., Nonino, Mario, Pirzkal, Nor, Robotham, Aaron, Ryan, Jr., Russell E., Ortiz III, Rafael, Tompkins, Scott, Willmer, Christopher N. A., Yan, Haojing, and Holwerda, Benne W.
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Astrophysics - Astrophysics of Galaxies - Abstract
A wealth of observations have long suggested that the vast majority of isolated classical dwarf galaxies ($M_*=10^7$-$10^9$ M$_\odot$) are currently star-forming. However, recent observations of the large abundance of "Ultra-Diffuse Galaxies" beyond the reach of previous large spectroscopic surveys suggest that our understanding of the dwarf galaxy population may be incomplete. Here we report the serendipitous discovery of an isolated quiescent dwarf galaxy in the nearby Universe, which was imaged as part of the PEARLS GTO program. Remarkably, individual red-giant branch stars are visible in this near-IR imaging, suggesting a distance of $30\pm4$ Mpc, and a wealth of archival photometry point to an sSFR of $2\times10^{-11}$ yr$^{-1}$ and SFR of $4\times10^{-4}$ M$_\odot$ yr$^{-1}$. Spectra obtained with the Lowell Discovery Telescope find a recessional velocity consistent with the Hubble Flow and ${>}1500$ km/s separated from the nearest massive galaxy in SDSS, suggesting that this galaxy was either quenched from internal mechanisms or had a very high-velocity ($>1000$ km/s) interaction with a nearby massive galaxy in the past. This analysis highlights the possibility that many nearby quiescent dwarf galaxies are waiting to be discovered and that JWST has the potential to resolve them., Comment: Accepted to ApJ Letters
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- 2023
19. The JWST Discovery of the Triply-imaged Type Ia 'Supernova H0pe' and Observations of the Galaxy Cluster PLCK G165.7+67.0
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Frye, Brenda L., Pascale, Massimo, Pierel, Justin, Chen, Wenlei, Foo, Nicholas, Leimbach, Reagen, Garuda, Nikhil, Cohen, Seth, Kamieneski, Patrick, Windhorst, Rogier, Koekemoer, Anton M., Kelly, Pat, Summers, Jake, Engesser, Michael, Liu, Daizhong, Furtak, Lukas, Polletta, Maria, Harrington, Kevin, Willner, Steve, Diego, Jose M., Jansen, Rolf, Coe, Dan, Conselice, Christopher J., Dai, Liang, Dole, Herve, D'Silva, Jordan C. J., Driver, Simon, Grogin, Norman, Marshall, Madeline A., Meena, Ashish, Nonino, Mario, Ortiz III, Rafael, Pirzkal, Nor, Robotham, Aaron, Ryan, Russell E., Strolger, Lou, Tompkins, Scott, Trussler, James, Willmer, Christopher, Yan, Haojing, Yun, Min S., and Zitrin, Adi
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Astrophysics - Astrophysics of Galaxies - Abstract
A Type Ia supernova (SN) at $z=1.78$ was discovered in James Webb Space Telescope Near Infrared Camera imaging of the galaxy cluster PLCK G165.7+67.0 (G165; $z = 0.35$). The SN is situated 1.5-2 kpc from the host-galaxy nucleus and appears in three different locations as a result of gravitational lensing by G165. These data can yield a value for Hubble's constant using time delays from this multiply-imaged SN Ia that we call "SN H0pe." Over the cluster, we identified 21 image multiplicities, confirmed five of them using the Near-Infrared Spectrograph, and constructed a new lens model that gives a total mass within 600 kpc of ($2.6 \pm 0.3) \times 10^{14}$ $M_{\odot}$. The photometry uncovered a galaxy overdensity coincident with the SN host galaxy. NIRSpec confirmed six member galaxies, four of which surround the SN host galaxy with relative velocity $\lesssim$900 km s$^{-1}$ and projected physical extent $\lesssim$33 kpc. This compact galaxy group is dominated by the SN host galaxy, which has a stellar mass of $(5.0 \pm 0.1) \times 10^{11}$ $M_{\odot}$. The group members have specific star-formation rates of 2-260 Gyr$^{-1}$ derived from the H$\alpha$-line fluxes corrected for stellar absorption, dust extinction, and slit losses. Another group centered on a strongly-lensed dusty star forming galaxy is at $z=2.24$. The total (unobscured and obscured) SFR of this second galaxy group is estimated to be ($\gtrsim$100 $M_{\odot}$ yr$^{-1}$), which translates to a supernova rate of $\sim$1 SNe yr$^{-1}$, suggesting that regular monitoring of this cluster may yield additional SNe., Comment: 29 pages, Accepted to ApJ on November 24, 2023
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- 2023
20. EPOCHS IX. When cosmic dawn breaks: Evidence for evolved stellar populations in $7 < z < 12$ galaxies from PEARLS GTO and public NIRCam imaging
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Trussler, James A. A., Conselice, Christopher J., Adams, Nathan, Austin, Duncan, Ferreira, Leonardo, Harvey, Tom, Li, Qiong, Vijayan, Aswin P., Wilkins, Stephen M., Windhorst, Rogier A., Bhatawdekar, Rachana, Cheng, Cheng, Coe, Dan, Cohen, Seth H., Driver, Simon P., Frye, Brenda, Grogin, Norman A., Hathi, Nimish, Jansen, Rolf A., Koekemoer, Anton, Marshall, Madeline A., Nonino, Mario, Ortiz, Rafael, Pirzkal, Nor, Robotham, Aaron, Ryan Jr., Russell E., D'Silva, Jordan C. J., Summers, Jake, Tompkins, Scott, Willmer, Christopher N. A., and Yan, Haojing
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Astrophysics - Astrophysics of Galaxies - Abstract
The presence of evolved stars in high-redshift galaxies can place valuable indirect constraints on the onset of star formation in the Universe. Thus we use PEARLS GTO and public NIRCam photometric data to search for Balmer-break candidate galaxies at $7 < z < 12$. We find that our Balmer-break candidates at $z \sim 10.5$ tend to be older (115 Myr), have lower inferred [O III] + H$\beta$ emission line equivalent widths (120 \r{A}), have lower specific star formation rates (6 Gyr$^{-1}$) and redder UV slopes ($\beta = -1.8$) than our control sample of galaxies. However, these trends all become less strong at $z \sim 8$, where the F444W filter now probes the strong rest-frame optical emission lines, thus providing additional constraints on the current star formation activity of these galaxies. Indeed, the bursty nature of Epoch of Reionisation galaxies can lead to a disconnect between their current SED profiles and their more extended star-formation histories. We discuss how strong emission lines, the cumulative effect of weak emission lines, dusty continua and AGN can all contribute to the photometric excess seen in the rest-frame optical, thus mimicking the signature of a Balmer break. Additional medium-band imaging will thus be essential to more robustly identify Balmer-break galaxies. However, the Balmer break alone cannot serve as a definitive proxy for the stellar age of galaxies, being complexly dependent on the star-formation history. Ultimately, deep NIRSpec continuum spectroscopy and MIRI imaging will provide the strongest indirect constraints on the formation era of the first galaxies in the Universe, thereby revealing when cosmic dawn breaks., Comment: 25 pages, 16 figures, 2 tables. Updated to published version in MNRAS
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- 2023
21. A search for high-redshift direct-collapse black hole candidates in the PEARLS north ecliptic pole field
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Nabizadeh, Armin, Zackrisson, Erik, Pacucci, Fabio, Maksym, Peter W., Li, Weihui, Civano, Francesca, Cohen, Seth H., D'Silva, Jordan C. J., Koekemoer, Anton M., Summers, Jake, Windhorst, Rogier A., Adams, Nathan, Conselice, Christopher J., Coe, Dan, Driver, Simon P., Frye, Brenda, Grogin, Norman A., Jansen, Rolf A., Marshall, Madeline A., Nonino, Mario, Pirzkal, Nor, Robotham, Aaron, Rutkowski, Michael J., Ryan, Jr., Russell E., Tompkins, Scott, Willmer, Christopher N. A., Yan, Haojing, Diego, Jose M., Cheng, Cheng, Finkelstein, Steven L., Willner, S. P., Zitrin, Adi, Bhatawdekar, Rachana, and Gim, Hansung B.
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Astrophysics - Astrophysics of Galaxies ,Astrophysics - Cosmology and Nongalactic Astrophysics ,Astrophysics - High Energy Astrophysical Phenomena - Abstract
Direct-collapse black holes (DCBHs) of mass $\sim 10^4$-$10^5 {M}_\odot$ that form in HI-cooling halos in the early Universe are promising progenitors of the $\gtrsim 10^9 {M}_\odot$ supermassive black holes that fuel observed $z \gtrsim 7$ quasars. Efficient accretion of the surrounding gas onto such DCBH seeds may render them sufficiently bright for detection with the JWST up to $z\approx 20$. Additionally, the very steep and red spectral slope predicted across the $\approx 1$-5 $\mu$m wavelength range of the JWST/NIRSpec instrument during their initial growth phase should make them photometrically identifiable up to very high redshifts. In this work, we present a search for such DCBH candidates across the 34 arcmin$^{2}$ in the first two spokes of the JWST cycle-1 PEARLS survey of the north ecliptic pole time-domain field covering eight NIRCam filters down to a maximum depth of $\sim$ 29 AB mag. We identify two objects with spectral energy distributions consistent with the Pacucci et al. (2016) DCBH models. However, we also note that even with data in eight NIRCam filters, objects of this type remain degenerate with dusty galaxies and obscured active galactic nuclei over a wide range of redshifts. Follow-up spectroscopy would be required to pin down the nature of these objects. Based on our sample of DCBH candidates and assumptions on the typical duration of the DCBH steep-slope state, we set a conservative upper limit of $\lesssim 5\times 10^{-4}$ comoving Mpc$^{-3}$ (cMpc$^{-3}$) on the comoving density of host halos capable of hosting DCBHs with spectral energy distributions similar to the Pacucci et al. (2016) models at $z\approx 6$-14., Comment: 10 pages, 6 figures, 1 table, accepted for publication in A&A
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- 2023
22. JWST's PEARLS: Mothra, a new kaiju star at z=2.091 extremely magnified by MACS0416, and implications for dark matter models
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Diego, J. M., Sun, Bangzheng, Yan, Haojing, Furtak, Lukas J., Zackrisson, Erik, Dai, Liang, Kelly, Patrick, Nonino, Mario, Adams, Nathan, Meena, Ashish K., Willner, S. P., Zitrin, Adi, Cohen, Seth H., Silva, Jordan C. J. D, Jansen, Rolf A., Summers, Jake, Windhorst, Rogier A., Coe, Dan, Conselice, Christopher J., Driver, Simon P., Frye, Brenda, Grogin, Norman A., Koekemoer, Anton M., Marshall, Madeline A., Pirzkal, Nor, Robotham, Aaron, Rutkowski, Michael J., Ryan, Jr., Russell E., Tompkins, Scott, Willmer, Christopher N. A., and Bhatawdekar, Rachana
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Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
We report the discovery of Mothra, an extremely magnified monster star, likely a binary system of two supergiant stars, in one of the strongly lensed galaxies behind the galaxy cluster MACS0416. The star is in a galaxy with spectroscopic redshift $z=2.091$ in a portion of the galaxy that is parsecs away from the cluster caustic. The binary star is observed only on the side of the critical curve with negative parity but has been detectable for at least eight years, implying the presence of a small lensing perturber. Microlenses alone cannot explain the earlier observations of this object made with the Hubble Space Telescope. A larger perturber with a mass of at least $10^4$\,\Msun\ offers a more satisfactory explanation. Based on the lack of perturbation on other nearby sources in the same arc, the maximum mass of the perturber is $M< 2.5\times10^6$\,\Msun, making it the smallest substructure constrained by lensing above redshift 0.3. The existence of this millilens is fully consistent with the expectations from the standard cold dark matter model. On the other hand, the existence of such small substructure in a cluster environment has implications for other dark matter models. In particular, warm dark matter models with particle masses below 8.7\,keV are excluded by our observations. Similarly, axion dark matter models are consistent with the observations only if the axion mass is in the range $0.5\times10^{-22}\, {\rm eV} < m_a < 5\times10^{-22}\, {\rm eV}$., Comment: 26 pages and 27 figures
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- 2023
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23. JWST's PEARLS: Transients in the MACS J0416.1-2403 Field
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Yan, Haojing, Ma, Zhiyuan, Sun, Bangzheng, Wang, Lifan, Kelly, Patrick, Diego, Jose M., Cohen, Seth H., Windhorst, Rogier A., Jansen, Rolf A., Grogin, Norman A., Beacom, John F., Conselice, Christopher J., Driver, Simon P., Frye, Brenda, Coe, Dan, Marshall, Madeline A., Koekemoer, Anton, Willmer, Christopher N. A., Robotham, Aaron, D'Silva, Jordan C. J., Summers, Jake, Nonino, Mario, Pirzkal, Nor, Ryan, Jr., Russell E., Ortiz III, Rafael, Tompkins, Scott, Bhatawdekar, Rachana A., Cheng, Cheng, Zitrin, Adi, and Willner, S. P.
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Astrophysics - Astrophysics of Galaxies ,High Energy Physics - Experiment - Abstract
With its unprecedented sensitivity and spatial resolution, the James Webb Space Telescope (JWST) has opened a new window for time-domain discoveries in the infrared. Here we report observations in the only field that has received four epochs (spanning 126 days) of JWST NIRCam observations in Cycle 1. This field is towards MACS J0416.1-2403, which is a rich galaxy cluster at redshift z=0.4 and is one of the Hubble Frontier Fields. We have discovered 14 transients from these data. Twelve of these transients happened in three galaxies (with z=0.94, 1.01, and 2.091) crossing a lensing caustic of the cluster,and these transients are highly magnified by gravitational lensing. These 12 transients are likely of similar nature to those previously reported based on the Hubble Space Telescope (HST) data in this field, i.e., individual stars in the highly magnified arcs. However, these twelve could not have been found by HST because they are too red and too faint. The other two transients are associated with background galaxies (z=2.205 and 0.7093) that are only moderately magnified, and they are likely supernovae. They indicate a de-magnified supernova surface density, when monitored at a time cadence of a few months to a ~3--4 micron survey limit of AB ~ 28.5 mag, of ~0.5 per sq. arcmin integrated to z ~ 2. This survey depth is beyond the capability of HST but can be easily reached by JWST., Comment: ApJS accepted
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- 2023
24. EPOCHS VII: Discovery of high redshift ($6.5 < z < 12$) AGN candidates in JWST ERO and PEARLS data
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Juodžbalis, Ignas, Conselice, Christopher J., Singh, Maitrayee, Adams, Nathan, Ormerod, Katherine, Harvey, Thomas, Austin, Duncan, Volonteri, Marta, Cohen, Seth H., Jansen, Rolf A., Summers, Jake, Windhorst, Rogier A., D'Silva, Jordan C. J., Koekemoer, Anton M., Coe, Dan, Driver, Simon P., Frye, Brenda, Grogin, Norman A., Marshall, Madeline A., Nonino, Mario, Pirzkal, Nor, Robotham, Aaron, Ryan, Jr., Russell E., Ortiz III, Rafael, Tompkins, Scott, Willmer, Christopher N. A., and Yan, Haojing
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Astrophysics - Astrophysics of Galaxies - Abstract
We present an analysis of a sample of robust high redshift galaxies selected photometrically from the `blank' fields of the Prime Extragalactic Areas for Reionization Science (PEARLS) survey and Early Release Observations (ERO) data of the James Webb Space Telescope (JWST) with the aim of selecting candidate high redshift active galactic nuclei (AGN). Sources were identified from the parent sample using a threefold selection procedure, which includes spectral energy distribution (SED) fitting to identify sources that are best fitted by AGN SED templates, a further selection based on the relative performance of AGN and non-AGN models, and finally morphological fitting to identify compact sources of emission, resulting in a purity-oriented procedure. Using this procedure, we identify a sample of nine AGN candidates at $6.5 < z < 12$, from which we constrain their physical properties as well as measure a lower bound on the AGN fraction in this redshift range of $5 \pm 1$\%. As this is an extreme lower limit due to our focus on purity and our SEDs being calibrated for unobscured Type 1 AGN, this demonstrates that AGN are perhaps quite common at this early epoch. The rest-frame UV colors of our candidate objects suggest that these systems are potentially candidate obese black hole galaxies (OBG), or AGN with very little galaxy component. We also investigate emission from our sample sources from fields overlapping with Chandra and VLA surveys, allowing us to place X-ray and 3 GHz radio detection limits on our candidates. Of note is a $z = 11.9$ candidate source exhibiting an abrupt morphological shift in the reddest band as compared to the bluer bands, indicating a potential merger or an unusually strong outflow., Comment: Accepted by MNRAS, 12 pages, 11 figures, updated to the final accepted version
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- 2023
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25. Residential Smart Ventilation: A Review
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Walker, IS, Guyot, G, Sherman, M, and Jordan, C
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- 2023
26. Associations of luteal phase changes in vagally mediated heart rate variability with premenstrual emotional changes
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Katja M. Schmalenberger, Tory A. Eisenlohr-Moul, Marc N. Jarczok, Ekaterina Schneider, Jordan C. Barone, Julian F. Thayer, and Beate Ditzen
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Menstrual cycle ,Progesterone ,Vagally mediated heart rate variability ,Negative affect ,Gynecology and obstetrics ,RG1-991 ,Public aspects of medicine ,RA1-1270 - Abstract
Abstract Background A recent meta-analysis revealed that vagally mediated heart rate variability (vmHRV; a biomarker of emotion regulation capacity) significantly decreases in the luteal phase of the menstrual cycle. As two follow-up studies suggest, these vmHRV decreases are driven primarily by increased luteal progesterone (P4). However, analyses also revealed significant interindividual differences in vmHRV reactivity to the cycle, which is in line with longstanding evidence for interindividual differences in mood sensitivity to the cycle. The present study begins to investigate whether these interindividual differences in vmHRV cyclicity can explain who is at higher risk of showing premenstrual emotional changes. We expected a greater degree of midluteal vmHRV decrease to be predictive of a greater premenstrual increase in negative affect. Methods We conducted an observational study with a naturally cycling community sample (N = 31, M = 26.03 years). Over a span of six weeks, participants completed (a) daily ratings of negative affect and (b) counterbalanced lab visits in their ovulatory, midluteal, and perimenstrual phases. Lab visits were scheduled based on positive ovulation tests and included assessments of baseline vmHRV and salivary ovarian steroid levels. Results In line with previous research, multilevel models suggest that most of the sample shows ovulatory-to-midluteal vmHRV decreases which, however, were not associated with premenstrual emotional changes. Interestingly, it was only the subgroup with luteal increases in vmHRV whose negative affect markedly worsened premenstrually and improved postmenstrually. Conclusion The present study begins to investigate cyclical changes in vmHRV as a potential biomarker of mood sensitivity to the menstrual cycle. The results demonstrate a higher level of complexity in these associations than initially expected, given that only atypical midluteal increases in vmHRV are associated with greater premenstrual negative affect. Potential underlying mechanisms are discussed, among those the possibility that luteal vmHRV increases index compensatory efforts to regulate emotion in those with greater premenstrual negative affect. However, future studies with larger and clinical samples and more granular vmHRV assessments should build on these findings and further explore associations between vmHRV cyclicity and menstrually related mood changes.
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- 2024
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27. Embodying Hope on the Dance Floor
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Grasso, Jordan C.
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- 2024
28. Hidden giants in JWST's PEARLS: An ultra-massive z=4.26 sub-millimeter galaxy that is invisible to HST
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Smail, Ian, Dudzeviciute, Ugne, Gurwell, Mark, Fazio, Giovanni G., Willner, S. P., Swinbank, A. M., Arumugam, Vinodiran, Summers, Jake, Cohen, Seth H., Jansen, Rolf A., Windhorst, Rogier A., Meena, Ashish, Zitrin, Adi, Keel, William C., Coe, Dan, Conselice, Christopher J., D'Silva, Jordan C. J., Driver, Simon P., Frye, Brenda, Grogin, Norman A., Koekemoer, Anton M., Marshall, Madeline A., Nonino, Mario, Pirzkal, Nor, Robotham, Aaron, Rutkowski, Michael J., Ryan Jr., Russell E., Tompkins, Scott, Willmer, Christopher N. A., Yan, Haojing, Broadhurst, Thomas J., Cheng, Cheng, Diego, Jose M., Kamieneski, Patrick, and Yun, Min
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Astrophysics - Astrophysics of Galaxies - Abstract
We present a multi-wavelength analysis using SMA, JCMT, NOEMA, JWST, HST, and SST of two dusty strongly star-forming galaxies, 850.1 and 850.2, seen through the massive cluster lens A1489. These SMA-located sources both lie at z=4.26 and have bright dust continuum emission, but 850.2 is a UV-detected Lyman-break galaxy, while 850.1 is undetected at <2um, even with deep JWST/NIRCam observations. We investigate their stellar, ISM, and dynamical properties, including a pixel-level SED analysis to derive sub-kpc-resolution stellar-mass and Av maps. We find that 850.1 is one of the most massive and highly obscured, Av~5, galaxies known at z>4 with M*~10^11.8 Mo (likely forming at z>6), and 850.2 is one of the least massive and least obscured, Av~1, members of the z>4 dusty star-forming population. The diversity of these two dust-mass-selected galaxies illustrates the incompleteness of galaxy surveys at z>3-4 based on imaging at <2um, the longest wavelengths feasible from HST or the ground. The resolved mass map of 850.1 shows a compact stellar mass distribution, Re(mass)~1kpc, but its expected evolution to z~1.5 and then z~0 matches both the properties of massive, quiescent galaxies at z~1.5 and ultra-massive early-type galaxies at z~0. We suggest that 850.1 is the central galaxy of a group in which 850.2 is a satellite that will likely merge in the near future. The stellar morphology of 850.1 shows arms and a linear bar feature which we link to the active dynamical environment it resides within., Comment: Submitted to ApJ, comments welcome!
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- 2023
29. GAMA/DEVILS: Cosmic star formation and AGN activity over 12.5 billion years
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D'Silva, Jordan C. J., Driver, Simon P., Lagos, Claudia D. P., Robotham, Aaron S. G., Bellstedt, Sabine, Davies, Luke J. M., Thorne, Jessica E., Bland-Hawthorn, Joss, Bravo, Matias, Holwerda, Benne, Phillipps, Steven, Seymour, Nick, Siudek, Malgorzata, and Windhorst, Rogier A.
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Astrophysics - Astrophysics of Galaxies - Abstract
We use the Galaxy and Mass Assembly (GAMA) and the Deep Extragalactic Visible Legacy Survey (DEVILS) observational data sets to calculate the cosmic star formation rate (SFR) and active galactic nuclei (AGN) bolometric luminosity history (CSFH/CAGNH) over the last 12.5 billion years. SFRs and AGN bolometric luminosities were derived using the spectral energy distribution fitting code ProSpect, which includes an AGN prescription to self consistently model the contribution from both AGN and stellar emission to the observed rest-frame ultra-violet to far-infrared photometry. We find that both the CSFH and CAGNH evolve similarly, rising in the early Universe up to a peak at look-back time $\approx 10$~Gyr ($z \approx 2$), before declining toward the present day. The key result of this work is that we find the ratio of CAGNH to CSFH has been flat ($\approx 10^{42.5}\mathrm{erg \, s^{-1}M_{\odot}^{-1}yr}$) for $11$~Gyr up to the present day, indicating that star formation and AGN activity have been coeval over this time period. We find that the stellar masses of the galaxies that contribute most to the CSFH and CAGNH are similar, implying a common cause, which is likely gas inflow. The depletion of the gas supply suppresses cosmic star formation and AGN activity equivalently to ensure that they have experienced similar declines over the last 10 Gyr. These results are an important milestone for reconciling the role of star formation and AGN activity in the life cycle of galaxies., Comment: 16 pages, 10 figures. Figures 9 and 10 are the main results. Accepted for publication in Monthly Notices of the Royal Astronomical Society
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- 2023
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30. Magellanic System Stars Identified in SMACS J0723.3-7327 James Webb Space Telescope Early Release Observations Images
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Summers, Jake, Windhorst, Rogier A., Cohen, Seth H., Jansen, Rolf A., Carleton, Timothy, Kamieneski, Patrick S., Holwerda, Benne W., Conselice, Christopher J., Adams, Nathan J., Frye, Brenda, Diego, Jose M., Willmer, Christopher N. A., Ortiz III, Rafael, Cheng, Cheng, Pigarelli, Alex, Robotham, Aaron, D'Silva, Jordan C. J., Tompkins, Scott, Driver, Simon P., Yan, Haojing, Coe, Dan, Grogin, Norman, Koekemoer, Anton, Marshall, Madeline A., Pirzkal, Nor, and Ryan Jr, Russell E.
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Astrophysics - Astrophysics of Galaxies - Abstract
We identify 71 distant stars in JWST/NIRCam ERO images of the field of galaxy cluster SMACS J0723.3-7327 (SMACS 0723). Given the relatively small ($\sim$$10^{\circ}$) angular separation between SMACS 0723 and the Large Magellanic Cloud, it is likely that these stars are associated with the LMC outskirts or Leading Arm. This is further bolstered by a spectral energy distribution analysis, which suggests an excess of stars at a physical distance of $40-100$ kpc, consistent with being associated with or located behind the Magellanic system. In particular, we find that the overall surface density of stars brighter than 27.0 mag in the field of SMACS 0723 is $\sim$2.3 times that of stars in a blank field with similar galactic latitude (the North Ecliptic Pole Time Domain Field), and that the density of stars in the SMACS 0723 field with SED-derived distances consistent with the Magellanic system is $\sim$6.1 times larger than that of the blank field. The candidate stars at these distances are consistent with a stellar population at the same distance modulus with [Fe/H] $= -1.0$ and an age of $\sim$$5.0$ Gyr. On the assumption that all of the 71 stars are associated with the LMC, then the stellar density of the LMC at the location of the SMACS 0723 field is $\sim$$740$ stars kpc$^{-3}$, which helps trace the density of stars in the LMC outskirts., Comment: Published in ApJ
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- 2023
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31. A renewed search for radio emission from the variable $\gamma$-ray pulsar PSR J2021$+$4026
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Shaw, B., Stappers, B. W., Weltevrede, P., Jordan, C. A., Mickaliger, M. B., and Lyne, A. G.
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Astrophysics - High Energy Astrophysical Phenomena - Abstract
We undertake the first targeted search at 1.5 GHz for radio emission from the variable $\gamma$-ray pulsar PSR J2021$+$4026. This radio-quiet pulsar assumes one of two stable $\gamma$-ray emission states, between which it transitions on a timescale of years. These transitions, in both $\gamma$-ray flux and pulse profile shape, are accompanied by contemporaneous changes to the pulsar's spin-down rate. A number of radio pulsars are known to exhibit similar correlated variability, which in some cases involves an emission state in which the radio emission ceases to be detectable. In this paper, we perform a search for radio emission from PSR J2021$+$4026, using archival radio observations recorded when the pulsar was in each of its emission/spin-down states. Using improved techniques, we search for periodic radio emission as well as single pulse phenomena such as giant radio pulses and RRAT-like emission. Our search reveals no evidence of radio emission from PSR J2021$+$4026. We estimate that the flux density for periodic emission from PSR J2021$+$4026 does not exceed 0.2 mJy at this frequency. We also estimate single-pulse flux limits for RRAT-like bursts and giant radio pulses to be 0.3 and 100 Jy respectively. We discuss the transitioning behaviour of PSR J2021$+$4026 in the context of pulsar glitches, intermittent pulsars and the increasingly common emission-rotation correlation observed in radio pulsars., Comment: 10 pages, 5 figures, 3 tables
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- 2023
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32. EPOCHS Paper II: The Ultraviolet Luminosity Function from $7.5<z<13.5$ using 180 square arcminutes of deep, blank-fields from the PEARLS Survey and Public JWST data
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Adams, Nathan J., Conselice, Christopher J., Austin, Duncan, Harvey, Thomas, Ferreira, Leonardo, Trussler, James, Juodzbalis, Ignas, Li, Qiong, Windhorst, Rogier, Cohen, Seth H., Jansen, Rolf, Summers, Jake, Tompkins, Scott, Driver, Simon P., Robotham, Aaron, D'Silva, Jordan C. J., Yan, Haojing, Coe, Dan, Frye, Brenda, Grogin, Norman A., Koekemoer, Anton M., Marshall, Madeline A., Pirzkal, Nor, Ryan, Jr., Russell E., Maksym, W. Peter, Rutkowski, Michael J., Willmer, Christopher N. A., Hammel, Heidi B., Nonino, Mario, Bhatawdekar, Rachana, Wilkins, Stephen M., Bradley, Larry D., Broadhurst, Tom, Cheng, Cheng, Dole, Herve, Hathi, Nimish P., and Zitrin, Adi
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Astrophysics - Astrophysics of Galaxies - Abstract
We present an analysis of the ultraviolet luminosity function (UV LF) and star formation rate density of distant galaxies ($7.5 < z < 13.5$) in the `blank' fields of the Prime Extragalactic Areas for Reionization Science (PEARLS) survey combined with Early Release Science (ERS) data from the CEERS, GLASS, NGDEEP surveys/fields and the first data release of JADES. We use strict quality cuts on EAZY photometric redshifts to obtain a reliable selection and characterisation of high-redshift ($z>6.5$) galaxies from a consistently processed set of deep, near-infrared imaging. Within an area of 180 arcmin$^{2}$, we identify 1046 candidate galaxies at redshifts $z>6.5$ and we use this sample to study the ultraviolet luminosity function (UV LF) in four redshift bins between $7.5
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- 2023
33. Distinct Features of Plasma Ultrashort Single-Stranded Cell-Free DNA as Biomarkers for Lung Cancer Detection
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Cheng, Jordan C, Swarup, Neeti, Li, Feng, Kordi, Misagh, Lin, Chien-Chung, Yang, Szu-Chun, Huang, Wei-Lun, Aziz, Mohammad, Kim, Yong, Chia, David, Yeh, Yu-Min, Wei, Fang, Zheng, David, Zhang, Liying, Pellegrini, Matteo, Su, Wu-Chou, and Wong, David TW
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liquid biopsy ,uscfDNA ,cell-free DNA ,ultrashort cell-free DNA ,single-stranded - Abstract
BackgroundUsing broad range cell-free DNA sequencing (BRcfDNA-Seq), a nontargeted next-generation sequencing (NGS) methodology, we previously identified a novel class of approximately 50 nt ultrashort single-stranded cell-free DNA (uscfDNA) in plasma that is distinctly different from 167 bp mononucleosomal cell-free DNA (mncfDNA). We hypothesize that uscfDNA possesses characteristics that are useful for disease detection.MethodsUsing BRcfDNA-Seq, we examined both cfDNA populations in the plasma of 18 noncancer controls and 14 patients with late-stage nonsmall cell lung carcinoma (NSCLC). In comparison to mncfDNA, we assessed whether functional element (FE) peaks, fragmentomics, end-motifs, and G-Quadruplex (G-Quad) signatures could be useful features of uscfDNA for NSCLC determination.ResultsIn noncancer participants, compared to mncfDNA, uscfDNA fragments showed a 45.2-fold increased tendency to form FE peaks (enriched in promoter, intronic, and exonic regions), demonstrated a distinct end-motif-frequency profile, and presented with a 4.9-fold increase in G-Quad signatures. Within NSCLC participants, only the uscfDNA population had discoverable FE peak candidates. Additionally, uscfDNA showcased different end-motif-frequency candidates distinct from mncfDNA. Although both cfDNA populations showed increased fragmentation in NSCLC, the G-Quad signatures were more discriminatory in uscfDNA. Compilation of cfDNA features using principal component analysis revealed that the first 5 principal components of both cfDNA subtypes had a cumulative explained variance of >80%.ConclusionsThese observations indicate that the distinct biological processes of uscfDNA and that FE peaks, fragmentomics, end-motifs, and G-Quad signatures are uscfDNA features with promising biomarker potential. These findings further justify its exploration as a distinct class of biomarker to augment pre-existing liquid biopsy approaches.
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- 2023
34. Shone Complex: A Case Report of Congenital Heart Disease Detected Using Point-of-care Ultrasound
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Seaback, Jordan C., Masneri, David A., and Schoeneck, Jacob H.
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case report ,Shone complex ,point-of-care ultrasound ,cardiogenic shock ,congenital heart disease - Abstract
Introduction: Undiagnosed congenital heart disease and management of pediatric cardiogenic shock presents a diagnostic challenge for the emergency clinician. These diagnoses are rare and require a high index of suspicion given the overlap with more common pediatric pathology. Point-of-care ultrasound can assist in differentiating these presentations. We present a case of neonatal cardiogenic shock secondary to a previously undiagnosed congenital heart disease, specifically Shone complex, detected using point-of-care ultrasound. Case Report: A six-week-old female presented with severe respiratory distress and was found to be in cardiogenic shock secondary to a previously undiagnosed congenital heart defect.Conclusion: Initial diagnosis of congenital heart disease is uncommon in the emergency department, but it should be recognized by clinicians given the high associated morbidity and mortality. Point-of-care ultrasound is a powerful tool to assist in evaluating for cardiac abnormalities as an etiology for undifferentiated shock in the pediatric population.
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- 2023
35. Prognostication and Treatment-Limiting Decisions After Severe Traumatic Brain Injury
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Petitt, Jordan C., Kashkoush, Ahmed, Kelly, Michael L., Coccolini, Federico, Series Editor, Coimbra, Raul, Series Editor, Kirkpatrick, Andrew W., Series Editor, Di Saverio, Salomone, Series Editor, Ansaloni, Luca, Editorial Board Member, Balogh, Zsolt, Editorial Board Member, Biffl, Walt, Editorial Board Member, Catena, Fausto, Editorial Board Member, Davis, Kimberly, Editorial Board Member, Ferrada, Paula, Editorial Board Member, Fraga, Gustavo, Editorial Board Member, Ivatury, Rao, Editorial Board Member, Kluger, Yoram, Editorial Board Member, Leppaniemi, Ari, Editorial Board Member, Maier, Ron, Editorial Board Member, Moore, Ernest E., Editorial Board Member, Napolitano, Lena, Editorial Board Member, Peitzman, Andrew, Editorial Board Member, Reilly, Patrick, Editorial Board Member, Rizoli, Sandro, Editorial Board Member, Sakakushev, Boris E., Editorial Board Member, Sartelli, Massimo, Editorial Board Member, Scalea, Thomas, Editorial Board Member, Spain, David, Editorial Board Member, Stahel, Philip, Editorial Board Member, Sugrue, Michael, Editorial Board Member, Velmahos, George, Editorial Board Member, Weber, Dieter, Editorial Board Member, Brogi, Etrusca, editor, Ley, Eric J., editor, and Valadka, Alex, editor
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- 2024
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36. Associations of luteal phase changes in vagally mediated heart rate variability with premenstrual emotional changes
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Schmalenberger, Katja M., Eisenlohr-Moul, Tory A., Jarczok, Marc N., Schneider, Ekaterina, Barone, Jordan C., Thayer, Julian F., and Ditzen, Beate
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- 2024
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37. Distant relatives of a eukaryotic cell-specific toxin family evolved a complement-like mechanism to kill bacteria
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Abrahamsen, Hunter L., Sanford, Tristan C., Collamore, Casie E., Johnstone, Bronte A., Coyne, Michael J., García-Bayona, Leonor, Christie, Michelle P., Evans, Jordan C., Farrand, Allison J., Flores, Katia, Morton, Craig J., Parker, Michael W., Comstock, Laurie E., and Tweten, Rodney K.
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- 2024
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38. Inhomogeneous Galactic Chemical Evolution: Modelling Ultra-Faint Dwarf Galaxies of the Large Magellanic Cloud
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Alexander, R. K., Vincenzo, F., Ji, A. P., Richstein, H., Jordan, C. J., and Gibson, B. K.
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Astrophysics - Astrophysics of Galaxies ,Astrophysics - Cosmology and Nongalactic Astrophysics ,Astrophysics - Solar and Stellar Astrophysics - Abstract
Ultra-faint dwarf galaxies are among the oldest and most metal-poor galaxies in the cosmos, observed to contain no gas and a high dark matter mass fraction. Understanding the chemical abundance dispersion in such extreme environments could shed light on the very first generations of stars. We present a novel inhomogeneous chemical evolution model, {\tt i-GEtool}, that we apply to two ultra-faint dwarf galaxies, Carina II and Reticulum II, both satellites of the Large Magellanic Cloud. Our model is based on the Monte Carlo sampling of the initial mass function as star formation proceeds in different gas cells of the galaxy volume. We account for the chemical enrichment of Supernova bubbles as they spread in the interstellar medium, causing dispersion in the elemental abundances. We recreate the abundance patterns of $\alpha$- and odd-$\textit{Z}$ elements, predicting two sequences in [C/Fe] and [N/Fe] at all metallicities. Our models underestimate [C/Fe] and [Ti/Fe] because of the large uncertainty in the adopted stellar nucleosynthesis yields. We discuss that the observed C and N abundances had likely been affected by internal mixing processes, which changed the initial surface abundances in the red giants. Our Supernova feedback scheme is responsible for driving galactic outflows, which quench the star formation activity at early times. We predict an average outflow mass-loading factor $\approx 10^{3}$, which extrapolates towards very low galaxy stellar masses the trend observed at high masses. Finally, by combining our model with the MIST isochrone database, we compare our synthetic colour-magnitude diagrams to observations., Comment: 19 Pages, 12 Figures, 1 Table, Accepted to MNRAS
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- 2023
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39. Hirsutonosema embarrassi n. gen. n. sp. (Phylum Microsporidia) in the Ovary of Mucket (Actinonaias ligamentina), Plain Pocketbook (Lampsilis cardium), and Fatmucket (Lampsilis siliquoidea) (Unionidae) from the Embarrass River, Wisconsin, USA
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Susan Knowles, Eric M. Leis, Jordan C. Richard, Isaac F. Standish, Jamie Bojko, Jesse Weinzinger, and Diane L. Waller
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Actinonaias ligamentina ,freshwater mussel ,Hirsutonosema embarrassi n. gen. n. sp. ,histopathology ,Lampsilis cardium ,Lampsilis siliquoidea ,Infectious and parasitic diseases ,RC109-216 ,Biology (General) ,QH301-705.5 - Abstract
During an epidemiological survey following a mortality event of freshwater mussels in 2018 in the Embarrass River, Wisconsin, USA, we identified a novel microsporidian parasite in the ovaries of mucket (Actinonaias ligamentina), plain pocketbook (Lampsilis cardium), and fatmucket (Lampsilis siliquoidea) (Unionidae). Histopathology showed round-to-oval microsporidian spores in the cytoplasm of oocytes in 60% (3/5) of female mucket, 100% (4/4) of female plain pocketbook, and 50% (1/2) of female fatmucket. Using transmission electron microscopy, we found that mature spores were round-to-oval and measured 4.13 ± 0.64 µm (3.14–5.31) long by 2.88 ± 0.37 µm (2.36–3.68) wide. The spores had a thin electron-dense exospore with a spiky “hairy” coat, a thick electron lucent endospore, diplokaryotic nuclei, a polar vacuole, and 27–28 polar filaments arranged in 1–3 rows. Sequencing of the small subunit rRNA produced a 1356 bp sequence most similar to that of Pseudonosema cristatellae (92%), and phylogenetic analysis grouped it within the freshwater Neopereziida. Genetic, morphological, and ultrastructural characteristics did not closely match those of other Pseudonosema spp., and a new genus and species, Hirsutonosema embarrassi n. gen. n. sp., were designated. Additional studies could evaluate host susceptibility, distribution, seasonality, transmission, and lethal or sub-lethal effects of this parasite on freshwater mussels.
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- 2024
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40. Distant relatives of a eukaryotic cell-specific toxin family evolved a complement-like mechanism to kill bacteria
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Hunter L. Abrahamsen, Tristan C. Sanford, Casie E. Collamore, Bronte A. Johnstone, Michael J. Coyne, Leonor García-Bayona, Michelle P. Christie, Jordan C. Evans, Allison J. Farrand, Katia Flores, Craig J. Morton, Michael W. Parker, Laurie E. Comstock, and Rodney K. Tweten
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Science - Abstract
Abstract Cholesterol-dependent cytolysins (CDCs) comprise a large family of pore-forming toxins produced by Gram-positive bacteria, which are used to attack eukaryotic cells. Here, we functionally characterize a family of 2-component CDC-like (CDCL) toxins produced by the Gram-negative Bacteroidota that form pores by a mechanism only described for the mammalian complement membrane attack complex (MAC). We further show that the Bacteroides CDCLs are not eukaryotic cell toxins like the CDCs, but instead bind to and are proteolytically activated on the surface of closely related species, resulting in pore formation and cell death. The CDCL-producing Bacteroides is protected from the effects of its own CDCL by the presence of a surface lipoprotein that blocks CDCL pore formation. These studies suggest a prevalent mode of bacterial antagonism by a family of two-component CDCLs that function like mammalian MAC and that are wide-spread in the gut microbiota of diverse human populations.
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- 2024
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41. Boolean Networks as Predictive Models of Emergent Biological Behaviors
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Rozum, Jordan C., Campbell, Colin, Newby, Eli, Nasrollahi, Fatemeh Sadat Fatemi, and Albert, Réka
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- 2024
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42. Correction to: Venous Interventions
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Ahmed, Syed Samaduddin, primary, Said, Adam, additional, Ahmed, Osman, additional, Lee, Patrick, additional, Madassery, Sreekumar, additional, Winokur, Ron, additional, Holly, Brian P., additional, Lessne, Mark, additional, Chan, Shin Mei, additional, Desai, Kush R., additional, Tasse, Jordan C., additional, Mcnamara, Griffin, additional, Drogin, Jillian, additional, and Pereira, Keith, additional
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- 2024
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43. Closing the gaps in adolescent vaccinations: Rhode Island’s Vaccinate Before You Graduate program as a model for other jurisdictions
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Dora M. Dumont, Jennifer S. Levy, Lisa M. Gargano, and Jordan C. White
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Immunization ,Vaccination ,Adolescents ,Preventive care ,Vaccinate Before You Graduate ,Disparities ,Medicine - Abstract
Objective: The northeastern state of Rhode Island (RI) has a Vaccinate Before You Graduate (VBYG) program that supplements the traditional primary care infrastructure by providing vaccines to adolescents while they are in school, with no out-of-pocket expenses. We analyzed data from RI’s immunization registry to evaluate whether VBYG also reduces disparities in adolescent immunization rates. Methods: We identified adolescent and catch-up vaccines administered in RI to people who were aged 11–18 at any point during the 5-year study period of 2019–2023, and conducted bivariate and multivariate analyses of vaccine administration data by setting (VBYG clinics, community health centers [CHCs], all other primary care practices [oPCPs], other school-based clinics, and other sites) and adolescent demographics (racial and ethnic identity, insurance status, sex, and age at time of vaccine). Results: Of over 387,000 routine vaccines administered during the study period, 3.3 % were administered by a VBYG clinic despite significant declines during school closures associated with the early COVID-19 pandemic. VBYG-administered doses went to slightly older youth, and a higher proportion were catch-up doses (25.7 % versus 14.1 % for CHC doses and 6.5 % for oPCP). Youths received an average of 2.71 vaccines in VBYG clinics compared to 1.77 from oPCPs and 2.08 from CHCs. A higher proportion of vaccines administered by VBYG went to adolescents of color and those without private insurance than those administered by oPCPs. Conclusions: VBYG provides a model to other jurisdictions of a vaccine safety net for adolescents who may not otherwise receive recommended vaccines before exiting the school system.
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- 2024
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44. Integrating developmental neuroscience with community-engaged approaches to address mental health outcomes for housing-insecure youth: Implications for research, practice, and policy
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Jordan C. Foster, H.R. Hodges, Anna Beloborodova, Emily M. Cohodes, Mirelle Q. Phillips, Erik Anderson, Bunmi Fagbenro, and Dylan G. Gee
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Early-life stress ,Housing insecurity ,Unpredictability ,Community-engaged research ,Policy ,Neurophysiology and neuropsychology ,QP351-495 - Abstract
One in three children in the United States is exposed to insecure housing conditions, including unaffordable, inconsistent, and unsafe housing. These exposures have detrimental impacts on youth mental health. Delineating the neurobehavioral pathways linking exposure to housing insecurity with children’s mental health has the potential to inform interventions and policy. However, in approaching this work, carefully considering the lived experiences of youth and families is essential to translating scientific discovery to improve health outcomes in an equitable and representative way. In the current paper, we provide an introduction to the range of stressful experiences that children may face when exposed to insecure housing conditions. Next, we highlight findings from the early-life stress literature regarding the potential neurobehavioral consequences of insecure housing, focusing on how unpredictability is associated with the neural circuitry supporting cognitive and emotional development. We then delineate how community-engaged research (CEnR) approaches have been leveraged to understand the effects of housing insecurity on mental health, and we propose future research directions that integrate developmental neuroscience research and CEnR approaches to maximize the impact of this work. We conclude by outlining practice and policy recommendations that aim to improve the mental health of children exposed to insecure housing.
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- 2024
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45. Estimation of maximum body size in fossil species: A case study using Tyrannosaurus rex
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Jordan C. Mallon and David W. E. Hone
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body mass ,dinosaurs ,ontogeny ,palaeoecology ,sexual size dimorphism ,Tyrannosauridae ,Ecology ,QH540-549.5 - Abstract
Abstract Among extant species, the ability to sample the extremes of body size—one of the most useful predictors of an individual's ecology—is highly unlikely. This improbability is further exaggerated when sampling the already incomplete fossil record. We quantify the likelihood of sampling the uppermost limits of body size in the fossil record using Tyrannosaurus rex Osborn, 1905 as a model, selected for its comparatively well‐understood life history parameters. We computationally generate a population of 140 million T. rex (based on prior estimates), modelling variation about the growth curve both with and without sexual dimorphism (the former modelled after Alligator mississippiensis), and building in sampling limitations related to species survivorship and taphonomic bias, derived from fossil data. The 99th percentile of body mass in T. rex has likely already been sampled, but it will probably be millennia before much larger giants (99.99th percentile) are sampled at present collecting rates. Biomechanical and ecological limitations notwithstanding, we estimate that the absolute largest T. rex may have been 70% more massive than the currently largest known specimen (~15,000 vs. ~8800 kg). Body size comparisons of fossil species should be based on ontogenetically controlled statistical parameters, rather than simply comparing the largest known individuals whose recovery is highly subject to sampling intensity.
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- 2024
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46. Inferring gene regulatory networks using transcriptional profiles as dynamical attractors
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Li, Ruihao, Rozum, Jordan C, Quail, Morgan M, Qasim, Mohammad N, Sindi, Suzanne S, Nobile, Clarissa J, Albert, Réka, and Hernday, Aaron D
- Subjects
Biochemistry and Cell Biology ,Bioinformatics and Computational Biology ,Genetics ,Biological Sciences ,Bioengineering ,Human Genome ,Generic health relevance ,Bayes Theorem ,Gene Regulatory Networks ,Algorithms ,Biological Evolution ,Candida albicans ,RNA ,Messenger ,Mathematical Sciences ,Information and Computing Sciences ,Bioinformatics - Abstract
Genetic regulatory networks (GRNs) regulate the flow of genetic information from the genome to expressed messenger RNAs (mRNAs) and thus are critical to controlling the phenotypic characteristics of cells. Numerous methods exist for profiling mRNA transcript levels and identifying protein-DNA binding interactions at the genome-wide scale. These enable researchers to determine the structure and output of transcriptional regulatory networks, but uncovering the complete structure and regulatory logic of GRNs remains a challenge. The field of GRN inference aims to meet this challenge using computational modeling to derive the structure and logic of GRNs from experimental data and to encode this knowledge in Boolean networks, Bayesian networks, ordinary differential equation (ODE) models, or other modeling frameworks. However, most existing models do not incorporate dynamic transcriptional data since it has historically been less widely available in comparison to "static" transcriptional data. We report the development of an evolutionary algorithm-based ODE modeling approach (named EA) that integrates kinetic transcription data and the theory of attractor matching to infer GRN architecture and regulatory logic. Our method outperformed six leading GRN inference methods, none of which incorporate kinetic transcriptional data, in predicting regulatory connections among TFs when applied to a small-scale engineered synthetic GRN in Saccharomyces cerevisiae. Moreover, we demonstrate the potential of our method to predict unknown transcriptional profiles that would be produced upon genetic perturbation of the GRN governing a two-state cellular phenotypic switch in Candida albicans. We established an iterative refinement strategy to facilitate candidate selection for experimentation; the experimental results in turn provide validation or improvement for the model. In this way, our GRN inference approach can expedite the development of a sophisticated mathematical model that can accurately describe the structure and dynamics of the in vivo GRN.
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- 2023
47. JWST's PEARLS: Prime Extragalactic Areas for Reionization and Lensing Science: Project Overview and First Results
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Windhorst, Rogier A., Cohen, Seth H., Jansen, Rolf A., Summers, Jake, Tompkins, Scott, Conselice, Christopher J., Driver, Simon P., Yan, Haojing, Coe, Dan, Frye, Brenda, Grogin, Norman, Koekemoer, Anton, Marshall, Madeline A., O'Brien, Rosalia, Pirzkal, Nor, Robotham, Aaron, Ryan, Jr., Russell E., Willmer, Christopher N. A., Carleton, Timothy, Diego, Jose M., Keel, William C., Porto, Paolo, Redshaw, Caleb, Scheller, Sydney, Wilkins, Stephen M., Willner, S. P., Zitrin, Adi, Adams, Nathan J., Austin, Duncan, Arendt, Richard G., Beacom, John F., Bhatawdekar, Rachana A., Bradley, Larry D., Broadhurst, Thomas J., Cheng, Cheng, Civano, Francesca, Dai, Liang, Dole, Herve, D'Silva, Jordan C. J., Duncan, Kenneth J., Fazio, Giovanni G., Ferrami, Giovanni, Ferreira, Leonardo, Finkelstein, Steven L., Furtak, Lukas J., Gim, Hansung B., Griffiths, Alex, Hammel, Heidi B., Harrington, Kevin C., Hathi, Nimish P., Holwerda, Benne W., Honor, Rachel, Huang, Jia-Sheng, Hyun, Minhee, Im, Myungshin, Joshi, Bhavin A., Kamieneski, Patrick S., Kelly, Patrick, Larson, Rebecca L., Li, Juno, Lim, Jeremy, Ma, Zhiyuan, Maksym, Peter, Manzoni, Giorgio, Meena, Ashish Kumar, Milam, Stefanie N., Nonino, Mario, Pascale, Massimo, Pierel, Justin D. R., Petric, Andreea, Polletta, Maria del Carmen, Rottgering, Huub J. A., Rutkowski, Michael J., Smail, Ian, Straughn, Amber N., Strolger, Louis-Gregory, Swirbul, Andi, Trussler, James A. A., Wang, Lifan, Welch, Brian, Wyithe, J. Stuart B., Yun, Min, Zackrisson, Erik, Zhang, Jiashuo, and Zhao, Xiurui
- Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics ,Astrophysics - Astrophysics of Galaxies - Abstract
We give an overview and describe the rationale, methods, and first results from NIRCam images of the JWST "Prime Extragalactic Areas for Reionization and Lensing Science" ("PEARLS") project. PEARLS uses up to eight NIRCam filters to survey several prime extragalactic survey areas: two fields at the North Ecliptic Pole (NEP); seven gravitationally lensing clusters; two high redshift proto-clusters; and the iconic backlit VV 191 galaxy system to map its dust attenuation. PEARLS also includes NIRISS spectra for one of the NEP fields and NIRSpec spectra of two high-redshift quasars. The main goal of PEARLS is to study the epoch of galaxy assembly, AGN growth, and First Light. Five fields, the JWST NEP Time-Domain Field (TDF), IRAC Dark Field (IDF), and three lensing clusters, will be observed in up to four epochs over a year. The cadence and sensitivity of the imaging data are ideally suited to find faint variable objects such as weak AGN, high-redshift supernovae, and cluster caustic transits. Both NEP fields have sightlines through our Galaxy, providing significant numbers of very faint brown dwarfs whose proper motions can be studied. Observations from the first spoke in the NEP TDF are public. This paper presents our first PEARLS observations, their NIRCam data reduction and analysis, our first object catalogs, the 0.9-4.5 $\mu$m galaxy counts and Integrated Galaxy Light. We assess the JWST sky brightness in 13 NIRCam filters, yielding our first constraints to diffuse light at 0.9-4.5 {\mu}m. PEARLS is designed to be of lasting benefit to the community., Comment: Accepted to AJ, comments welcome. We ask anyone who uses our public PEARLS (NEP TDF) data to refer to this overview paper
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- 2022
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48. Webb's PEARLS: Bright 1.5--2.0 micron Dropouts in the Spitzer/IRAC Dark Field
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Yan, Haojing, Cohen, Seth H., Windhorst, Rogier A., Jansen, Rolf A., Ma, Zhiyuan, Beacom, John F., Cheng, Cheng, Huang, Jia-Sheng, Grogin, Norman A., Willner, S. P., Yun, Min, Hammel, Heidi B., Milam, Stefanie N., Conselice, Christopher J., Driver, Simon P., Frye, Brenda, Marshall, Madeline A., Koekemoer, Anton, Willmer, Christopher N. A., Robotham, Aaron, D'Silva, Jordan C. J., Summers, Jake, Ling, Chenxiaoji, Lim, Jeremy, Harrington, Kevin, Ferreira, Leonardo, Diego, Jose Maria, Pirzkal, Nor, Wilkins, Stephen M., Wang, Lifan, Hathi, Nimish P., Zitrin, Adi, Bhatawdekar, Rachana A., Adams, Nathan J., Furtak, Lukas J., Maksym, Peter, Rutkowski, Michael J., and Fazio, Giovanni G.
- Subjects
Astrophysics - Astrophysics of Galaxies ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
Using the first epoch of four-band NIRCam observations obtained by the James Webb Space Telescope (JWST) Prime Extragalactic Areas for Reionization and Lensing Science Program in the Spitzer IRAC Dark Field, we search for F150W and F200W dropouts. In 14.2 arcmin^2, we have found eight F150W dropouts and eight F200W dropouts, all brighter than 27.5 mag (the brightest being ~24 mag) in the band to the red side of the break. As they are detected in multiple bands, these must be real objects. Their nature, however, is unclear, and characterizing their properties is important for realizing the full potential of JWST. If the observed color decrements are due to the Lyman break, these objects should be at z >~ 11.7 and z >~ 15.4, respectively. The color diagnostics show that at least four F150W dropouts are far away from the usual contaminators encountered in dropout searches (red galaxies at much lower redshifts or brown dwarf stars). While the diagnostics of the F200W dropouts are less certain due to the limited number of passbands, at least one of them is likely not a known type of contaminant, and the rest are consistent with either high-redshift galaxies with evolved stellar populations or old galaxies at z ~ 3 to 8. If a significant fraction of our dropouts are indeed at z ~ 12, we have to face the severe problem of explaining their high luminosities and number densities. Spectroscopic identifications of such objects are urgently needed., Comment: Accepted for publication in ApJL
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- 2022
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49. Unveiling the main sequence of galaxies at $z \geq 5$ with the James Webb Space Telescope: predictions from simulations
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D'Silva, Jordan C. J., Lagos, Claudia D. P., Davies, Luke J. M., Lovell, Christopher C., and Vijayan, Aswin P.
- Subjects
Astrophysics - Astrophysics of Galaxies - Abstract
We use two independent, galaxy formation simulations, FLARES, a cosmological hydrodynamical simulation, and SHARK, a semi-analytic model, to explore how well the James Webb Space Telescope (JWST) will be able to uncover the existence and parameters of the star-forming main sequence (SFS) at $z=5\to10$, i.e. shape, scatter, normalisation. Using two independent simulations allows us to isolate predictions (e.g., stellar mass, star formation rate, SFR, luminosity functions) that are robust to or highly dependent on the implementation of the physics of galaxy formation. Both simulations predict that JWST can observe $\ge 70-90\%$ (for SHARK and FLARES respectively) of galaxies up to $z\sim10$ (down to stellar masses of $\approx 10^{8.3}\,\rm M_{\odot}$ and SFRs of $\approx 10^{0.5}\,\rm M_{\odot}\, yr^{-1}$) in modest integration times and given current proposed survey areas (e.g. the Web COSMOS $0.6\,\rm deg^2$) to accurately constrain the parameters of the SFS. Although both simulations predict qualitatively similar distributions of stellar mass and SFR, there are important quantitative differences, such as the abundance of massive, star-forming galaxies, with FLARES predicting a higher abundance than SHARK; the early onset of quenching as a result of black hole growth in FLARES (at $z\approx 8$), not seen in SHARK until much lower redshifts; and the implementation of synthetic photometry, with FLARES predicting more JWST-detected galaxies ($\sim 90\%$) than SHARK ($\sim 70\%$) at $z=10$. JWST observations will distinguish between these models, leading to a significant improvement upon our understanding of the formation of the very first galaxies., Comment: 21 pages, 13 figures including 1 in appendix, accepted to MNRAS
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- 2022
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50. A measurement of small-scale features using ionospheric scintillation. Comparison with refractive shift measurements
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Waszewski, A., Morgan, J., and Jordan, C. H.
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Astrophysics - Instrumentation and Methods for Astrophysics - Abstract
We present a study of scintillation induced by the mid-latitude ionosphere. By implementing methods currently used in Interplanetary Scintillation studies to measure amplitude scintillation at low frequencies, we have proven it is possible to use the Murchison Widefield Array to study ionospheric scintillation in the weak regime, which is sensitive to structures on scales $\sim$300 m at our observing frequency of 154 MHz, where the phase variance on this scale was 0.06 rad$^{2}$ in the most extreme case observed. Analysing over 1000 individual 2-minute observations, we compared the ionospheric phase variance with that inferred with previous measurements of refractive shifts, which are most sensitive to scales almost an order of magnitude larger. The two measurements were found to be highly correlated (Pearson correlation coefficient 0.71). We observed that for an active ionosphere, the relationship between these two metrics is in line with what would be expected if the ionosphere's structure is described by Kolmogorov turbulence between the relevant scales of 300m and 2000m. In the most extreme ionospheric conditions, the refractive shifts were sometimes found to underestimate the small-scale variance by a factor of four or more, and it is these ionospheric conditions that could have significant effects on radio astronomy observations., Comment: 12 pages, 9 figures, 1 table, accepted for publication in PASA
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- 2022
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