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18 results on '"Cornwell, Daniel J"'

1. The localization of galaxy groups in close proximity to galaxy clusters using cosmic web nodes

Author

Cornwell, Daniel J., Kuchner, Ulrike, Gray, Meghan E., Aragón-Salamanca, Alfonso, Pearce, Frazer R., Cui, Weiguang, and Knebe, Alexander

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We investigate the efficacy of using the cosmic web nodes identified by the DisPerSE topological filament finder to systematically identify galaxy groups in the infall regions around massive clusters. The large random motions and infall velocities of galaxies in the regions around clusters complicate the detection and characterisation of substructures through normal group-finding algorithms. Yet understanding the co-location of galaxies within filaments and/or groups is a key part of understanding the role of environment on galaxy evolution, particularly in light of next-generation wide-field spectroscopic surveys. Here we use simulated massive clusters from TheThreeHundred collaboration and compare the derived group catalogues, (haloes with $\sigma_{v} > 300 h^{-1}$ km/s) with the critical points from DisPerSE, ran on haloes with more than 100 particles. We find that in 3D, 56\% of DisPerSE nodes are correctly identified as groups (purity) while 68\% of groups are identified as nodes (completeness). The fraction of matches increases with group mass and with distance from the host cluster centre. This rises to a completeness of 100\% for the most massive galaxy groups ($M>10^{14}$ M$_{\odot}$) in 3D, or 63\% when considering the projected 2D galaxy distribution. When a perfect match occurs between a cosmic web node and a galaxy group, the DisPerSE node density ($\delta$) serves as an estimate of the group's mass, albeit with significant scatter. We conclude that the use of a cosmic filament finder shows promise as a useful and straightforward observational tool for disentangling substructure within the infall regions of massive clusters., Comment: Accepted for publication in MNRAS

Published
2023

2. The probability of identifying the cosmic web environment of galaxies around clusters motivated by the Weave Wide Field Cluster Survey

Author

Cornwell, Daniel J., Aragón-Salamanca, Alfonso, Kuchner, Ulrike, Gray, Meghan E., Pearce, Frazer R., and Knebe, Alexander

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Upcoming wide-field spectroscopic surveys will observe galaxies in a range of cosmic web environments in and around galaxy clusters. In this paper, we test and quantify how successfully we will be able to identify the environment of individual galaxies in the vicinity of massive galaxy clusters, reaching out to $\sim5R_{200}$ into the clusters' infall region. We focus on the WEAVE Wide Field Cluster Survey (WWFCS), but the methods we develop can be easily generalised to any similar spectroscopic survey. Using numerical simulations of a large sample of massive galaxy clusters from \textsc{TheThreeHundred} project, we produce mock observations that take into account the selection effects and observational constraints imposed by the WWFCS. We then compare the `true' environment of each galaxy derived from the simulations (cluster core, filament, and neither core nor filament, {``NCF''}) with the one derived from the observational data, where only galaxy sky positions and spectroscopic redshifts will be available. We find that, while cluster core galaxy samples can be built with a high level of completeness and moderate contamination, the filament and NCF galaxy samples will be significantly contaminated and incomplete due to projection effects exacerbated by the galaxies' peculiar velocities. We conclude that, in the infall regions surrounding massive galaxy clusters, associating galaxies with the correct cosmic web environment is highly uncertain. However, with large enough spectroscopic samples like the ones the WWFCS will provide (thousands of galaxies per cluster, {out to $5R_{200}$}), and the correct statistical treatment that takes into account the probabilities we provide here, we expect we will be able to extract robust and well-quantified conclusions on the relationship between galaxy properties and their environment., Comment: Accepted for publication in MNRAS (14 pages, 7 figures)

Published
2023
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3. The wide-field, multiplexed, spectroscopic facility WEAVE: Survey design, overview, and simulated implementation

Author

Jin, Shoko, Trager, Scott C., Dalton, Gavin B., Aguerri, J. Alfonso L., Drew, J. E., Falcón-Barroso, Jesús, Gänsicke, Boris T., Hill, Vanessa, Iovino, Angela, Pieri, Matthew M., Poggianti, Bianca M., Smith, D. J. B., Vallenari, Antonella, Abrams, Don Carlos, Aguado, David S., Antoja, Teresa, Aragón-Salamanca, Alfonso, Ascasibar, Yago, Babusiaux, Carine, Balcells, Marc, Barrena, R., Battaglia, Giuseppina, Belokurov, Vasily, Bensby, Thomas, Bonifacio, Piercarlo, Bragaglia, Angela, Carrasco, Esperanza, Carrera, Ricardo, Cornwell, Daniel J., Domínguez-Palmero, Lilian, Duncan, Kenneth J., Famaey, Benoit, Fariña, Cecilia, Gonzalez, Oscar A., Guest, Steve, Hatch, Nina A., Hess, Kelley M., Hoskin, Matthew J., Irwin, Mike, Knapen, Johan H., Koposov, Sergey E., Kuchner, Ulrike, Laigle, Clotilde, Lewis, Jim, Longhetti, Marcella, Lucatello, Sara, Méndez-Abreu, Jairo, Mercurio, Amata, Molaeinezhad, Alireza, Monguió, Maria, Morrison, Sean, Murphy, David N. A., de Arriba, Luis Peralta, Pérez, Isabel, Pérez-Ràfols, Ignasi, Picó, Sergio, Raddi, Roberto, Romero-Gómez, Mercè, Royer, Frédéric, Siebert, Arnaud, Seabroke, George M., Som, Debopam, Terrett, David, Thomas, Guillaume, Wesson, Roger, Worley, C. Clare, Alfaro, Emilio J., Prieto, Carlos Allende, Alonso-Santiago, Javier, Amos, Nicholas J., Ashley, Richard P., Balaguer-Núñez, Lola, Balbinot, Eduardo, Bellazzini, Michele, Benn, Chris R., Berlanas, Sara R., Bernard, Edouard J., Best, Philip, Bettoni, Daniela, Bianco, Andrea, Bishop, Georgia, Blomqvist, Michael, Boeche, Corrado, Bolzonella, Micol, Bonoli, Silvia, Bosma, Albert, Britavskiy, Nikolay, Busarello, Gianni, Caffau, Elisabetta, Cantat-Gaudin, Tristan, Castro-Ginard, Alfred, Couto, Guilherme, Carbajo-Hijarrubia, Juan, Carter, David, Casamiquela, Laia, Conrado, Ana M., Corcho-Caballero, Pablo, Costantin, Luca, Deason, Alis, de Burgos, Abel, De Grandi, Sabrina, Di Matteo, Paola, Domínguez-Gómez, Jesús, Dorda, Ricardo, Drake, Alyssa, Dutta, Rajeshwari, Erkal, Denis, Feltzing, Sofia, Ferré-Mateu, Anna, Feuillet, Diane, Figueras, Francesca, Fossat, Matteo, Franciosin, Elena, Frasca, Antonio, Fumagalli, Michele, Gallazzi, Anna, García-Benito, Rubén, Fusillo, Nicola Gentile, Gebran, Marwan, Gilbert, James, Gledhill, T. M., Delgado, Rosa M. González, Greimel, Robert, Guarcello, Mario Giuseppe, Guerra, Jose, Gullieuszik, Marco, Haines, Christopher P., Hardcastle, Martin J., Harris, Amy, Haywood, Misha, Helmi, Amina, Hernandez, Nauzet, Herrero, Artemio, Hughes, Sarah, Irsic, Vid, Jablonka, Pascale, Jarvis, Matt J., Jordi, Carme, Kondapally, Rohit, Kordopatis, Georges, Krogager, Jens-Kristian, La Barbera, Francesco, Lam, Man I, Larsen, Søren S., Lemasle, Bertrand, Lewis, Ian J., Lhomé, Emilie, Lind, Karin, Lodi, Marcello, Longobardi, Alessia, Lonoce, Ilaria, Magrin, Laura, Apellániz, Jesús Maíz, Marchal, Olivier, Marco, Amparo, Martin, Nicolas F., Matsuno, Tadafumi, Maurogordato, Sophie, Merluzzi, Paola, Miralda-Escudé, Jordi, Molinari, Emilio, Monari, Giacomo, Morelli, Lorenzo, Mottram, Christopher J., Naylor, Tim, Negueruela, Ignacio, Oñorbe, Jose, Pancino, Elena, Peirani, Sébastien, Peletier, Reynier F., Pozzetti, Lucia, Rainer, Monica, Ramos, Pau, Read, Shaun C., Rossi, Elena Maria, Röttgering, Huub J. A., Rubiño-Martín, Jose Alberto, Montes, Jose Sabater, Juan, José San, Sanna, Nicoletta, Schallig, Ellen, Schiavon, Ricardo P., Schultheis, Mathias, Serra, Paolo, Shimwell, Timothy W., Simón-Díaz, Sergio, Smith, Russell J., Sordo, Rosanna, Sorini, Daniele, Soubiran, Caroline, Starkenburg, Else, Steele, Iain A., Stott, John, Stuik, Remko, Tolstoy, Eline, Tortora, Crescenzo, Tsantaki, Maria, Van der Swaelmen, Mathieu, van Weeren, Reinout J., Vergani, Daniela, Verheijen, Marc A. W., Verro, Kristiina, Vink, Jorick S., Vioque, Miguel, Walcher, C. Jakob, Walton, Nicholas A., Wegg, Christopher, Weijmans, Anne-Marie, Williams, Wendy L., Wilson, Andrew J., Wright, Nicholas J., Xylakis-Dornbusch, Theodora, Youakim, Kris, Zibetti, Stefano, and Zurita, Cristina

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - Solar and Stellar Astrophysics
Abstract

WEAVE, the new wide-field, massively multiplexed spectroscopic survey facility for the William Herschel Telescope, will see first light in late 2022. WEAVE comprises a new 2-degree field-of-view prime-focus corrector system, a nearly 1000-multiplex fibre positioner, 20 individually deployable 'mini' integral field units (IFUs), and a single large IFU. These fibre systems feed a dual-beam spectrograph covering the wavelength range 366$-$959\,nm at $R\sim5000$, or two shorter ranges at $R\sim20\,000$. After summarising the design and implementation of WEAVE and its data systems, we present the organisation, science drivers and design of a five- to seven-year programme of eight individual surveys to: (i) study our Galaxy's origins by completing Gaia's phase-space information, providing metallicities to its limiting magnitude for $\sim$3 million stars and detailed abundances for $\sim1.5$ million brighter field and open-cluster stars; (ii) survey $\sim0.4$ million Galactic-plane OBA stars, young stellar objects and nearby gas to understand the evolution of young stars and their environments; (iii) perform an extensive spectral survey of white dwarfs; (iv) survey $\sim400$ neutral-hydrogen-selected galaxies with the IFUs; (v) study properties and kinematics of stellar populations and ionised gas in $z<0.5$ cluster galaxies; (vi) survey stellar populations and kinematics in $\sim25\,000$ field galaxies at $0.3\lesssim z \lesssim 0.7$; (vii) study the cosmic evolution of accretion and star formation using $>1$ million spectra of LOFAR-selected radio sources; (viii) trace structures using intergalactic/circumgalactic gas at $z>2$. Finally, we describe the WEAVE Operational Rehearsals using the WEAVE Simulator., Comment: 41 pages, 27 figures, accepted for publication by MNRAS; updated version including information on individual grants in a revised Acknowledgements section, corrections to the affiliation list, and an updated references list

Published
2022
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4. Forecasting the success of the WEAVE Wide-Field Cluster Survey on the extraction of the cosmic web filaments around galaxy clusters

Author

Cornwell, Daniel J., Kuchner, Ulrike, Aragón-Salamanca, Alfonso, Gray, Meghan E., Pearce, Frazer R., Aguerri, J. Alfonso L., Cui, Weiguang, Méndez-Abreu, J., de Arriba, Luis Peralta, and Trager, Scott C.

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Next-generation wide-field spectroscopic surveys will observe the infall regions around large numbers of galaxy clusters with high sampling rates for the first time. Here we assess the feasibility of extracting the large-scale cosmic web around clusters using forthcoming observations, given realistic observational constraints. We use a sample of 324 hydrodynamic zoom-in simulations of massive galaxy clusters from TheThreeHundred project to create a mock-observational catalogue spanning $5R_{200}$ around 160 analogue clusters. These analogues are matched in mass to the 16 clusters targetted by the forthcoming WEAVE Wide-Field Cluster Survey (WWFCS). We consider the effects of the fibre allocation algorithm on our sampling completeness and find that we successfully allocate targets to 81.7 $\% \pm$ 1.3 of the members in the cluster outskirts. We next test the robustness of the filament extraction algorithm by using a metric, $D_{\text{skel}}$, which quantifies the distance to the filament spine. We find that the median positional offset between reference and recovered filament networks is $D_{\text{skel}} = 0.13 \pm 0.02$ Mpc, much smaller than the typical filament radius of $\sim$ 1 Mpc. Cluster connectivity of the recovered network is not substantially affected. Our findings give confidence that the WWFCS will be able to reliably trace cosmic web filaments in the vicinity around massive clusters, forming the basis of environmental studies into the effects of pre-processing on galaxy evolution., Comment: 18 pages, 14 figures. Accepted by MNRAS for publication

Published
2022
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7. The localization of galaxy groups in close proximity to galaxy clusters using cosmic web nodes.

Author

Cornwell, Daniel J, Kuchner, Ulrike, Gray, Meghan E, Aragón-Salamanca, Alfonso, Pearce, Frazer R, Cui, Weiguang, and Knebe, Alexander

Subjects
*GALAXY clusters, *LARGE scale structure (Astronomy), *GALACTIC evolution
Abstract

We investigate the efficacy of using the cosmic web nodes identified by the DisPerSE topological filament finder to systematically identify galaxy groups in the infall regions around massive clusters. The large random motions and infall velocities of galaxies in the regions around clusters complicate the detection and characterisation of substructures through normal group-finding algorithms. Yet understanding the co-location of galaxies within filaments and/or groups is a key part of understanding the role of environment on galaxy evolution, particularly in light of next-generation wide-field spectroscopic surveys. Here we use simulated massive clusters from TheThreeHundred collaboration and compare the derived group catalogues, (haloes with σ v > 300  h −1 km s−1) with the critical points from DisPerSE, ran on haloes with more than 100 particles. We find that in 3D, 56 per cent of DisPerSE nodes are correctly identified as groups (purity) while 68  per cent of groups are identified as nodes (completeness). The fraction of matches increases with group mass and with distance from the host cluster centre. This rises to a completeness of 100 per cent for the most massive galaxy groups (M > 1014 M⊙) in 3D, or 63 per cent when considering the projected 2D galaxy distribution. When a perfect match occurs between a cosmic web node and a galaxy group, the DisPerSE node density (δ) serves as an estimate of the group's mass, albeit with significant scatter. We conclude that the use of a cosmic filament finder shows promise as a useful and straightforward observational tool for disentangling substructure within the infall regions of massive clusters. [ABSTRACT FROM AUTHOR]

Published
2024
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9. The wide-field, multiplexed, spectroscopic facility WEAVE: Survey design, overview, and simulated implementation

Author

Jin, Shoko, primary, Trager, Scott C, additional, Dalton, Gavin B, additional, Aguerri, J Alfonso L, additional, Drew, J E, additional, Falcón-Barroso, Jesús, additional, Gänsicke, Boris T, additional, Hill, Vanessa, additional, Iovino, Angela, additional, Pieri, Matthew M, additional, Poggianti, Bianca M, additional, Smith, D J B, additional, Vallenari, Antonella, additional, Abrams, Don Carlos, additional, Aguado, David S, additional, Antoja, Teresa, additional, Aragón-Salamanca, Alfonso, additional, Ascasibar, Yago, additional, Babusiaux, Carine, additional, Balcells, Marc, additional, Barrena, R, additional, Battaglia, Giuseppina, additional, Belokurov, Vasily, additional, Bensby, Thomas, additional, Bonifacio, Piercarlo, additional, Bragaglia, Angela, additional, Carrasco, Esperanza, additional, Carrera, Ricardo, additional, Cornwell, Daniel J, additional, Domínguez-Palmero, Lilian, additional, Duncan, Kenneth J, additional, Famaey, Benoit, additional, Fari na, Cecilia, additional, Gonzalez, Oscar A, additional, Guest, Steve, additional, Hatch, Nina A, additional, Hess, Kelley M, additional, Hoskin, Matthew J, additional, Irwin, Mike, additional, Knapen, Johan H, additional, Koposov, Sergey E, additional, Kuchner, Ulrike, additional, Laigle, Clotilde, additional, Lewis, Jim, additional, Longhetti, Marcella, additional, Lucatello, Sara, additional, Méndez-Abreu, Jairo, additional, Mercurio, Amata, additional, Molaeinezhad, Alireza, additional, Monguió, Maria, additional, Morrison, Sean, additional, Murphy, David N A, additional, de Arriba, Luis Peralta, additional, Pérez, Isabel, additional, Pérez-Ràfols, Ignasi, additional, Picó, Sergio, additional, Raddi, Roberto, additional, Romero-Gómez, Mercè, additional, Royer, Frédéric, additional, Siebert, Arnaud, additional, Seabroke, George M, additional, Som, Debopam, additional, Terrett, David, additional, Thomas, Guillaume, additional, Wesson, Roger, additional, Worley, C Clare, additional, Alfaro, Emilio J, additional, Prieto, Carlos Allende, additional, Alonso-Santiago, Javier, additional, Amos, Nicholas J, additional, Ashley, Richard P, additional, Balaguer-Nú nez, Lola, additional, Balbinot, Eduardo, additional, Bellazzini, Michele, additional, Benn, Chris R, additional, Berlanas, Sara R, additional, Bernard, Edouard J, additional, Best, Philip, additional, Bettoni, Daniela, additional, Bianco, Andrea, additional, Bishop, Georgia, additional, Blomqvist, Michael, additional, Boeche, Corrado, additional, Bolzonella, Micol, additional, Bonoli, Silvia, additional, Bosma, Albert, additional, Britavskiy, Nikolay, additional, Busarello, Gianni, additional, Caffau, Elisabetta, additional, Cantat-Gaudin, Tristan, additional, Castro-Ginard, Alfred, additional, Couto, Guilherme, additional, Carbajo-Hijarrubia, Juan, additional, Carter, David, additional, Casamiquela, Laia, additional, Conrado, Ana M, additional, Corcho-Caballero, Pablo, additional, Costantin, Luca, additional, Deason, Alis, additional, de Burgos, Abel, additional, De Grandi, Sabrina, additional, Di Matteo, Paola, additional, Domínguez-Gómez, Jesús, additional, Dorda, Ricardo, additional, Drake, Alyssa, additional, Dutta, Rajeshwari, additional, Erkal, Denis, additional, Feltzing, Sofia, additional, Ferré-Mateu, Anna, additional, Feuillet, Diane, additional, Figueras, Francesca, additional, Fossati, Matteo, additional, Franciosini, Elena, additional, Frasca, Antonio, additional, Fumagalli, Michele, additional, Gallazzi, Anna, additional, García-Benito, Rubén, additional, Fusillo, Nicola Gentile, additional, Gebran, Marwan, additional, Gilbert, James, additional, Gledhill, T M, additional, Delgado, Rosa M González, additional, Greimel, Robert, additional, Guarcello, Mario Giuseppe, additional, Guerra, Jose, additional, Gullieuszik, Marco, additional, Haines, Christopher P, additional, Hardcastle, Martin J, additional, Harris, Amy, additional, Haywood, Misha, additional, Helmi, Amina, additional, Hernandez, Nauzet, additional, Herrero, Artemio, additional, Hughes, Sarah, additional, Irsic, Vid, additional, Jablonka, Pascale, additional, Jarvis, Matt J, additional, Jordi, Carme, additional, Kondapally, Rohit, additional, Kordopatis, Georges, additional, Krogager, Jens-Kristian, additional, Barbera, Francesco La, additional, Lam, Man I, additional, Larsen, Søren S, additional, Lemasle, Bertrand, additional, Lewis, Ian J, additional, Lhomé, Emilie, additional, Lind, Karin, additional, Lodi, Marcello, additional, Longobardi, Alessia, additional, Lonoce, Ilaria, additional, Magrini, Laura, additional, Apellániz, Jesús Maíz, additional, Marchal, Olivier, additional, Marco, Amparo, additional, Martin, Nicolas F, additional, Matsuno, Tadafumi, additional, Maurogordato, Sophie, additional, Merluzzi, Paola, additional, Miralda-Escudé, Jordi, additional, Molinari, Emilio, additional, Monari, Giacomo, additional, Morelli, Lorenzo, additional, Mottram, Christopher J, additional, Naylor, Tim, additional, Negueruela, Ignacio, additional, Onorbe, Jose, additional, Pancino, Elena, additional, Peirani, Sébastien, additional, Peletier, Reynier F, additional, Pozzetti, Lucia, additional, Rainer, Monica, additional, Ramos, Pau, additional, Read, Shaun C, additional, Rossi, Elena Maria, additional, Röttgering, Huub J A, additional, Rubi no-Martín, Jose Alberto, additional, Montes, Jose Sabater, additional, Juan, José San, additional, Sanna, Nicoletta, additional, Schallig, Ellen, additional, Schiavon, Ricardo P, additional, Schultheis, Mathias, additional, Serra, Paolo, additional, Shimwell, Timothy W, additional, Simón-Díaz, Sergio, additional, Smith, Russell J, additional, Sordo, Rosanna, additional, Sorini, Daniele, additional, Soubiran, Caroline, additional, Starkenburg, Else, additional, Steele, Iain A, additional, Stott, John, additional, Stuik, Remko, additional, Tolstoy, Eline, additional, Tortora, Crescenzo, additional, Tsantaki, Maria, additional, Van der Swaelmen, Mathieu, additional, van Weeren, Reinout J, additional, Vergani, Daniela, additional, Verheijen, Marc A W, additional, Verro, Kristiina, additional, Vink, Jorick S, additional, Vioque, Miguel, additional, Walcher, C Jakob, additional, Walton, Nicholas A, additional, Wegg, Christopher, additional, Weijmans, Anne-Marie, additional, Williams, Wendy L, additional, Wilson, Andrew J, additional, Wright, Nicholas J, additional, Xylakis-Dornbusch, Theodora, additional, Youakim, Kris, additional, Zibetti, Stefano, additional, and Zurita, Cristina, additional

Published
2023
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10. Forecasting the success of the WEAVE Wide-Field Cluster Survey on the extraction of the cosmic web filaments around galaxy clusters

Author

Cornwell, Daniel J, primary, Kuchner, Ulrike, additional, Aragón-Salamanca, Alfonso, additional, Gray, Meghan E, additional, Pearce, Frazer R, additional, Aguerri, J Alfonso L, additional, Cui, Weiguang, additional, Méndez-Abreu, J, additional, Peralta de Arriba, Luis, additional, and Trager, Scott C, additional

Published
2022
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12. 1,3:2,4-Dibenzylidene-d-sorbitol (DBS) and its derivatives-efficient, versatile and industrially-relevant low-molecular-weight gelators with over 100 years of history and a bright future

Author

Okesola, Babatunde O., Vieira, Vânia M P, Cornwell, Daniel J., Whitelaw, Nicole K., and Smith, David K.

Abstract

Dibenzylidene-d-sorbitol (DBS) has been a well-known low-molecular-weight gelator of organic solvents for over 100 years. As such, it constitutes a very early example of a supramolecular gel-a research field which has recently developed into one of intense interest. The ability of DBS to self-assemble into sample-spanning networks in numerous solvents is predicated upon its 'butterfly-like' structure, whereby the benzylidene groups constitute the 'wings' and the sorbitol backbone the 'body'-the two parts representing the molecular recognition motifs underpinning its gelation mechanism, with the nature of solvent playing a key role in controlling the precise assembly mode. This gelator has found widespread applications in areas as diverse as personal care products and polymer nucleation/clarification, and has considerable potential in applications such as dental composites, energy technology and liquid crystalline materials. Some derivatives of DBS have also been reported which offer the potential to expand the scope and range of applications of this family of gelators and endow the nansocale network with additional functionality. This review aims to explain current trends in DBS research, and provide insight into how by combining a long history of application, with modern methods of derivatisation and analysis, the future for this family of gelators is bright, with an increasing number of high-tech applications, from environmental remediation to tissue engineering, being within reach.

Published
2015

17. 1,3:2,4-Dibenzylidene-D-sorbitol (DBS) and its derivatives--efficient, versatile and industrially-relevant low-molecular-weight gelators with over 100 years of history and a bright future.

Author

Okesola BO, Vieira VM, Cornwell DJ, Whitelaw NK, and Smith DK

Abstract

Dibenzylidene-D-sorbitol (DBS) has been a well-known low-molecular-weight gelator of organic solvents for over 100 years. As such, it constitutes a very early example of a supramolecular gel--a research field which has recently developed into one of intense interest. The ability of DBS to self-assemble into sample-spanning networks in numerous solvents is predicated upon its 'butterfly-like' structure, whereby the benzylidene groups constitute the 'wings' and the sorbitol backbone the 'body'--the two parts representing the molecular recognition motifs underpinning its gelation mechanism, with the nature of solvent playing a key role in controlling the precise assembly mode. This gelator has found widespread applications in areas as diverse as personal care products and polymer nucleation/clarification, and has considerable potential in applications such as dental composites, energy technology and liquid crystalline materials. Some derivatives of DBS have also been reported which offer the potential to expand the scope and range of applications of this family of gelators and endow the nansocale network with additional functionality. This review aims to explain current trends in DBS research, and provide insight into how by combining a long history of application, with modern methods of derivatisation and analysis, the future for this family of gelators is bright, with an increasing number of high-tech applications, from environmental remediation to tissue engineering, being within reach.

Published
2015
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18. Multidomain hybrid hydrogels: spatially resolved photopatterned synthetic nanomaterials combining polymer and low-molecular-weight gelators.

Author

Cornwell DJ, Okesola BO, and Smith DK

Subjects
Diffusion, Hydrogen-Ion Concentration, Kinetics, Nanostructures ultrastructure, Photochemical Processes, Polymers chemistry, Hydrogels chemistry, Nanostructures chemistry
Abstract

A simple approach to a patterned multidomain gel is reported, combining a pH-responsive low-molecular-weight gelator (LMWG) and a photoinducible polymer gelator (PG). Using SEM (scanning electron microscopy), NMR spectroscopy, and CD, we demonstrate that self-assembly of the LMWG network occurs in the presence of the PG network, but that the PG has an influence on LMWG assembly kinetics and morphology. The application of a mask during photoirradiation allows patterning of the PG network; we define the resulting system as a "multidomain gel"-one domain consists of a LMWG, whereas the patterned region contains both LMWG and PG networks. The different domains have different properties with regard to diffusion of small molecules, and both gelator networks can control diffusion rates to give systems capable of controlled release. Such materials may have future applications in multikinetic control of drug release, or as patterned scaffolds for directed tissue engineering., (© 2014 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim.)

Published
2014
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