Exploring and interrogating astrophysical data in virtual reality

Jarrett, T. H.; Comrie, A.; Marchetti, L.; Sivitilli, Alexander K.; Macfarlane, S.; Vitello, F.; Taylor, Andrew; Hulst, J. M. van der; Serra, P.; Katz, Neal; Cluver, Michelle

doi:10.1016/j.ascom.2021.100502

Cited by 15 publications

(8 citation statements)

References 39 publications

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“…Having obtained the 98 H i mosaic cube, we run SoFiA manually outside CARACal to create a better clean mask. We verify that this mask includes all (and only) real H i emission detectable on various angular and velocity scales through visual inspection of 2D cube slices as well as in virtual reality (iDaVIE; Jarrett et al 2021). We use this clean mask to make our final 98 H i cubes, which we then combine into our final 98 H i mosaic.…”

Section: H I Mosaicsmentioning

confidence: 76%

The MeerKAT Fornax Survey

Serra¹,

Maccagni²,

Kleiner³

et al. 2023

A&A

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The MeerKAT Fornax Survey maps the distribution and kinematics of atomic neutral hydrogen gas (H i) in the nearby Fornax galaxy cluster using the MeerKAT telescope. The 12 deg 2 survey footprint covers the central region of the cluster out to ∼ R vir and stretches out to ∼ 2R vir towards south west to include the NGC 1316 galaxy group. The H i column density sensitivity (3σ over 25 km s −1 ) ranges from 5 × 10 19 cm −2 at a resolution of ∼ 10 (∼ 1 kpc at the 20 Mpc distance of Fornax) down to ∼ 10 18 cm −2 at ∼ 1 (∼ 6 kpc), and slightly below this level at the lowest resolution of ∼ 100 (∼ 10 kpc). The H i mass sensitivity (3σ over 50 km s −1 ) is 6 × 10 5 M . The H i velocity resolution is 1.4 km s −1 . In this paper we describe the survey design and H i data processing, and we present a sample of six galaxies with long, one-sided, star-less H i tails (of which only one was previously known) radially oriented within the cluster and with measurable internal velocity gradients. We argue that the joint properties of the H i tails represent the first unambiguous evidence of ram pressure shaping the distribution of H i in the Fornax cluster. The disturbed optical morphology of all host galaxies supports the idea that the tails consist of H i initially pulled out of the galaxies' stellar body by tidal forces. Ram pressure was then able to further displace the weakly bound H i and give the tails their present direction, length and velocity gradient.

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Section: H I Mosaicsmentioning

confidence: 76%

The MeerKAT Fornax Survey

Serra¹,

Maccagni²,

Kleiner³

et al. 2023

A&A

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“…Printed versions of these 3D renderings, together with their visualization in virtual reality experiences connected to the physical processes investigated (see Orlando et al 2019), will allow us to pursue a more inclusive scientific environment by increasing the accessibility of Rubin LSSTʼs results for blind and visually impaired researchers. Moreover, thanks to their interactive and immersive nature (e.g., Jarrett et al 2021), these tools will also prove invaluable in assisting the broader community of astronomers in their exploration and research of the complex astrophysical systems that can be investigated with Vera C. Rubin Observatory LSST.…”

Section: Discussionmentioning

confidence: 99%

Young Stellar Objects, Accretion Disks, and Their Variability with Rubin Observatory LSST

Bonito

Venuti

Ustamujic

et al. 2023

ApJS

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Vera C. Rubin Observatory, through the Legacy Survey of Space and Time (LSST), will allow us to derive a panchromatic view of variability in young stellar objects (YSOs) across all relevant timescales. Indeed, both short-term variability (on timescales of hours to days) and long-term variability (months to years), predominantly driven by the dynamics of accretion processes in disk-hosting YSOs, can be explored by taking advantage of the multiband filters option available in Rubin LSST, in particular the u, g, r, i filters that enable us to discriminate between photospheric stellar properties and accretion signatures. The homogeneity and depth of sky coverage that will be achieved with LSST will provide us with a unique opportunity to characterize the time evolution of disk accretion as a function of age and varying environmental conditions (e.g., field crowdedness, massive neighbors, metallicity) by targeting different star-forming regions. In this contribution to the Rubin LSST Survey Strategy Optimization Focus Issue, we discuss how implementing a dense observing cadence to explore short-term variability in YSOs represents a key complementary effort to the Wide–Fast–Deep observing mode that will be used to survey the sky over the full duration of the main survey (≈10 yr). The combination of these two modes will be vital to investigate the connection between the inner-disk dynamics and longer-term eruptive variability behaviors, such as those observed on EX Lupi–type objects.

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“…Consequently, we used a new visualisation tool to identify and divide the local maxima into seven discrete sources. Developed specifically for spectral-imaging data interaction, and notably with H i cubes, the Virtual Reality (VR) based software suite called iDaVIE 1 (Jarrett et al 2021) was deployed to separate the seven sources using mask-editing functionality in which the VR user is able to create (or modify) a mask that specifies which H i intensity voxels (3D pixels) belong to which sources. More details of this mask editing procedure and the resulting mask that was used to extract the source characterization is presented in Appendix B.…”

Section: H I Properties Of the Dark Cloud Chainmentioning

confidence: 99%

“…We deployed a new cutting edge visualisation tool to investigate the dark cloud chain. Designed specifically to work with spectral-imaging cubes, iDaVIE (Immersive Data Visualization Interactive Explorer 5 ) renders cubes in a room-scale 3D Virtual Reality (VR) space, where the user can intuitively view and uniquely interact with their data cube (Jarrett et al 2021). The software suite is designed to work with FITS cubes and products from the SoFiA 6 (Serra et al 2015) source finding package, including the mask cubes and extracted source lists.…”

Section: B Vr Visualisation Of the Dark Cloud Chainmentioning

confidence: 99%

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The detection of a massive chain of dark HI clouds in the GAMA G23 Field

Jozsa,

Jarrett,

Cluver

et al. 2021

Preprint

Self Cite

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We report on the detection of a large, extended H i cloud complex in the GAMA G23 field, located at a redshift of z ∼ 0.03, observed as part of the MeerHOGS campaign (a pilot survey to explore the mosaicing capabilities of MeerKAT). The cloud complex, with a total mass of 10 10.0 M , lies in proximity to a large galaxy group with M dyn ∼ 10 13.5 M . We identify seven H i peak concentrations, interconnected as a tenuous 'chain' structure, extending ∼400 kpc from east-to-west, with the largest (central) concentration containing 10 9.7 M in H i gas distributed across 50 kpc. The main source is not detected in ultra-violet, optical or infrared imaging. The implied gas mass-to-light (M HI /L r ) is extreme (>1000) even in comparison to other 'dark clouds'. The complex has very little kinematic structure (110 km s −1 ), making it difficult to identify cloud rotation. Assuming pressure support, the total mass of the central concentration is > 10 10.2 M , while a lower limit to the dynamical mass in the case of full rotational support is 10 10.4 M . If the central concentration is a stable structure, it has to contain some amount of unseen matter, but potentially less than is observed for a typical galaxy. It is, however, not clear whether the structure has any gravitationally stable concentrations. We report a faint UV-optical-infrared source in proximity to one of the smaller concentrations in the gas complex, leading to a possible stellar association. The system nature and origins is enigmatic, potentially being the result of an interaction with or within the galaxy group it appears to be associated with.

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Exploring and interrogating astrophysical data in virtual reality

Cited by 15 publications

References 39 publications

The MeerKAT Fornax Survey

The MeerKAT Fornax Survey

Young Stellar Objects, Accretion Disks, and Their Variability with Rubin Observatory LSST

The detection of a massive chain of dark HI clouds in the GAMA G23 Field

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