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2. Multiorgan MRI findings after hospitalisation with COVID-19 in the UK (C-MORE): a prospective, multicentre, observational cohort study
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Raman, Betty, McCracken, Celeste, Cassar, Mark P, Moss, Alastair J, Finnigan, Lucy, Samat, Azlan Helmy A, Ogbole, Godwin, Tunnicliffe, Elizabeth M, Alfaro-Almagro, Fidel, Menke, Ricarda, Xie, Cheng, Gleeson, Fergus, Lukaschuk, Elena, Lamlum, Hanan, McGlynn, Kevin, Popescu, Iulia A, Sanders, Zeena-Britt, Saunders, Laura C, Piechnik, Stefan K, Ferreira, Vanessa M, Nikolaidou, Chrysovalantou, Rahman, Najib M, Ho, Ling-Pei, Harris, Victoria C, Shikotra, Aarti, Singapuri, Amisha, Pfeffer, Paul, Manisty, Charlotte, Kon, Onn M, Beggs, Mark, O'Regan, Declan P, Fuld, Jonathan, Weir-McCall, Jonathan R, Parekh, Dhruv, Steeds, Rick, Poinasamy, Krisnah, Cuthbertson, Dan J, Kemp, Graham J, Semple, Malcolm G, Horsley, Alexander, Miller, Christopher A, O'Brien, Caitlin, Shah, Ajay M, Chiribiri, Amedeo, Leavy, Olivia C, Richardson, Matthew, Elneima, Omer, McAuley, Hamish J C, Sereno, Marco, Saunders, Ruth M, Houchen-Wolloff, Linzy, Greening, Neil J, Bolton, Charlotte E, Brown, Jeremy S, Choudhury, Gourab, Diar Bakerly, Nawar, Easom, Nicholas, Echevarria, Carlos, Marks, Michael, Hurst, John R, Jones, Mark G, Wootton, Daniel G, Chalder, Trudie, Davies, Melanie J, De Soyza, Anthony, Geddes, John R, Greenhalf, William, Howard, Luke S, Jacob, Joseph, Man, William D-C, Openshaw, Peter J M, Porter, Joanna C, Rowland, Matthew J, Scott, Janet T, Singh, Sally J, Thomas, David C, Toshner, Mark, Lewis, Keir E, Heaney, Liam G, Harrison, Ewen M, Kerr, Steven, Docherty, Annemarie B, Lone, Nazir I, Quint, Jennifer, Sheikh, Aziz, Zheng, Bang, Jenkins, R Gisli, Cox, Eleanor, Francis, Susan, Halling-Brown, Mark, Chalmers, James D, Greenwood, John P, Plein, Sven, Hughes, Paul J C, Thompson, A A Roger, Rowland-Jones, Sarah L, Wild, James M, Kelly, Matthew, Treibel, Thomas A, Bandula, Steven, Aul, Raminder, Miller, Karla, Jezzard, Peter, Smith, Stephen, Nichols, Thomas E, McCann, Gerry P, Evans, Rachael A, Wain, Louise V, Brightling, Christopher E, Neubauer, Stefan, Baillie, J K, Shaw, Alison, 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Beckett, P, Nanda, U, Daynes, E, Charalambou, A, Yousuf, A J, Lea, A, Prickett, A, Gooptu, Bibek, Hargadon, Beverley, Bourne, Charlotte, Christie, C, Edwardson, C, Lee, D, Baldry, E, Stringer, E, Woodhead, F, Mills, G, Arnold, H, Aung, H, Qureshi, I N, Finch, J, Skeemer, J, Hadley, K, Khunti, Kamlesh, Carr, Liesel, Ingram, L, Aljaroof, M, Bakali, M, Bakau, M, Baldwin, M, Bourne, Michelle, Pareek, Manish, Soares, M, Tobin, Martin, Armstrong, Natalie, Brunskill, Nigel, Goodman, N, Cairns, P, Haldar, Pranab, McCourt, P, Dowling, R, Russell, Richard, Diver, Sarah, Edwards, Sarah, Glover, Sarah, Parker, S, Siddiqui, Salman, Ward, T J C, Mcnally, T, Thornton, T, Yates, Tom, Ibrahim, W, Monteiro, Will, Thickett, D, Wilkinson, D, Broome, M, McArdle, P, Upthegrove, R, Wraith, D, Langenberg, C, Summers, C, Bullmore, E, Heeney, J L, Schwaeble, W, Sudlow, C L, Adeloye, D, Newby, D E, Rudan, I, Shankar-Hari, M, Thorpe, M, Pius, R, Walmsley, S, McGovern, A, Ballard, C, Allan, L, Dennis, J, Cavanagh, J, Petrie, J, O'Donnell, K, Spears, M, Sattar, N, MacDonald, S, Guthrie, E, Henderson, M, Guillen Guio, Beatriz, Zhao, Bang, Lawson, C, Overton, Charlotte, Taylor, Chris, Tong, C, Mukaetova-Ladinska, Elizabeta, Turner, E, Pearl, John E, Sargant, J, Wormleighton, J, Bingham, Michelle, Sharma, M, Steiner, Mike, Samani, Nilesh, Novotny, Petr, Free, Rob, Allen, R J, Finney, Selina, Terry, Sarah, Brugha, Terry, Plekhanova, Tatiana, McArdle, A, Vinson, B, Spencer, L G, Reynolds, W, Ashworth, M, Deakin, B, Chinoy, H, Abel, K, Harvie, M, Stanel, S, Rostron, A, Coleman, C, Baguley, D, Hufton, E, Khan, F, Hall, I, Stewart, I, Fabbri, L, Wright, L, Kitterick, P, Morriss, R, Johnson, S, Bates, A, Antoniades, C, Clark, D, Bhui, K, Channon, K M, Motohashi, K, Sigfrid, L, Husain, M, Webster, M, Fu, X, Li, X, Kingham, L, Klenerman, P, Miiler, K, Carson, G, Simons, G, Huneke, N, Calder, P C, Baldwin, D, Bain, S, Lasserson, D, Daines, L, Bright, E, Stern, M, Crisp, P, Dharmagunawardena, R, Reddington, A, Wight, A, Bailey, L, Ashish, A, Robinson, E, Cooper, J, Broadley, A, Turnbull, A, Brookes, C, Sarginson, C, Ionita, D, Redfearn, H, Elliott, K, Barman, L, Griffiths, L, Guy, Z, Gill, Rhyan, Nathu, Rashmita, Harris, Edward, Moss, P, Finnigan, J, Saunders, Kathryn, Saunders, Peter, Kon, S, Kon, Samantha S, O'Brien, Linda, Shah, K, Shah, P, Richardson, Emma, Brown, V, Brown, M, Brown, Jo, Brown, J, Brown, Ammani, Brown, Angela, Choudhury, N, Jones, S, Jones, H, Jones, L, Jones, I, Jones, G, Jones, Heather, Jones, Don, Davies, Ffyon, Davies, Ellie, Davies, Kim, Davies, Gareth, Davies, Gwyneth A, Howard, K, Porter, Julie, Rowland, J, Rowland, A, Scott, Kathryn, Singh, Suver, Singh, Claire, Thomas, S, Thomas, Caradog, Lewis, Victoria, Lewis, J, Lewis, D, Harrison, P, Francis, C, Francis, R, Hughes, Rachel Ann, Hughes, Joan, Hughes, A D, Thompson, T, Kelly, S, Smith, D, Smith, Nikki, Smith, Andrew, Smith, Jacqui, Smith, Laurie, Smith, Susan, Evans, Teriann, Evans, Ranuromanana I, Evans, D, Evans, R, Evans, H, and Evans, J
- Published
- 2023
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3. Effects of sleep disturbance on dyspnoea and impaired lung function following hospital admission due to COVID-19 in the UK: a prospective multicentre cohort study
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Jackson, C, Stewart, I D, Plekhanova, T, Cunningham, P S, Hazel, A L, Al-Sheklly, B, Aul, R, Bolton, C E, Chalder, T, Chalmers, J D, Chaudhuri, N, Docherty, A B, Donaldson, G, Edwardson, C L, Elneima, O, Greening, N J, Hanley, N A, Harris, V C, Harrison, E M, Ho, L-P, Houchen-Wolloff, L, Howard, L S, Jolley, C J, Jones, M G, Leavy, O C, Lewis, K E, Lone, N I, Marks, M, McAuley, H J C, McNarry, M A, Patel, B, Piper-Hanley, K, Poinasamy, K, Raman, B, Richardson, M, Rivera-Ortega, P, Rowland-Jones, S L, Rowlands, A V, Saunders, R M, Scott, J T, Sereno, M, Shah, A M, Shikotra, A, Singapuri, A, Stanel, S C, Thorpe, M, Wootton, D G, Yates, T, Jenkins, G, Singh, S J, Man, W D-C, Brightling, C E, Wain, L V, Porter, J C, Thompson, R, Horsley, A, Molyneaux, P L, Evans, R A, Jones, S E, Rutter, M K, Blaikley, J F, Abel, K, Adamali, H, Adeloye, D, Adeyemi, O, Adrego, R, Aguilar Jimenez, L A, Ahmad, S, Ahmad Haider, N, Ahmed, R, Ahwireng, N, Ainsworth, M, Alamoudi, A, Ali, M, Aljaroof, M, All, AM, Allan, L, Allen, R J, Allerton, L, Allsop, L, Almeida, P, Altmann, D, Alvarez Corral, M, Amoils, S, Anderson, D, Antoniades, C, Arbane, G, Arias, A, Armour, C, Armstrong, L, Armstrong, N, Arnold, D, Arnold, H, Ashish, A, Ashworth, A, Ashworth, M, Aslani, S, Assefa-Kebede, H, Atkin, C, Atkin, P, Aung, H, Austin, L, Avram, C, Ayoub, A, Babores, M, Baggott, R, Bagshaw, J, Baguley, D, Bailey, L, Baillie, J K, Bain, S, Bakali, M, Bakau, M, Baldry, E, Baldwin, D, Baldwin, M, Ballard, C, Banerjee, A, Bang, B, Barker, R E, Barman, L, Barratt, S, Barrett, F, Basire, D, Basu, N, Bates, M, Bates, A, Batterham, R, Baxendale, H, Bayes, H, Beadsworth, M, Beckett, P, Beggs, M, Begum, M, Beirne, P, Bell, D, Bell, R, Bennett, K, Beranova, E, Bermperi, A, Berridge, A, Berry, C, Betts, S, Bevan, E, Bhui, K, Bingham, M, Birchall, K, Bishop, L, Bisnauthsing, K, Blaikely, J, Bloss, A, Bolger, A, Bonnington, J, Botkai, A, Bourne, C, Bourne, M, Bramham, K, Brear, L, Breen, G, Breeze, J, Briggs, A, Bright, E, Brill, S, Brindle, K, Broad, L, Broadley, A, Brookes, C, Broome, M, Brown, A, Brown, J, Brown, J S, Brown, M, Brown, V, Brugha, T, Brunskill, N, Buch, M, Buckley, P, Bularga, A, Bullmore, E, Burden, L, Burdett, T, Burn, D, Burns, G, Burns, A, Busby, J, Butcher, R, Butt, A, Byrne, S, Cairns, P, Calder, P C, Calvelo, E, Carborn, H, Card, B, Carr, C, Carr, L, Carson, G, Carter, P, Casey, A, Cassar, M, Cavanagh, J, Chablani, M, Chambers, R C, Chan, F, Channon, K M, Chapman, K, Charalambou, A, Checkley, A, Chen, J, Cheng, Y, Chetham, L, Childs, C, Chilvers, E R, Chinoy, H, Chiribiri, A, Chong-James, K, Choudhury, G, Choudhury, N, Chowienczyk, P, Christie, C, Chrystal, M, Clark, D, Clark, C, Clarke, J, Clohisey, S, Coakley, G, Coburn, Z, Coetzee, S, Cole, J, Coleman, C, Conneh, F, Connell, D, Connolly, B, Connor, L, Cook, A, Cooper, B, Cooper, J, Cooper, S, Copeland, D, Cosier, T, Coulding, M, Coupland, C, Cox, E, Craig, T, Crisp, P, Cristiano, D, Crooks, M G, Cross, A, Cruz, I, Cullinan, P, Cuthbertson, D, Daines, L, Dalton, M, Daly, P, Daniels, A, Dark, P, Dasgin, J, David, A, David, C, Davies, E, Davies, F, Davies, G, Davies, G A, Davies, K, Davies, M J, Dawson, J, Daynes, E, De Soyza, A, Deakin, B, Deans, A, Deas, C, Deery, J, Defres, S, Dell, A, Dempsey, K, Denneny, E, Dennis, J, Dewar, A, Dharmagunawardena, R, Diar-Bakerly, N, Dickens, C, Dipper, A, Diver, S, Diwanji, S N, Dixon, M, Djukanovic, R, Dobson, H, Dobson, S L, Donaldson, A, Dong, T, Dormand, N, Dougherty, A, Dowling, R, Drain, S, Draxlbauer, K, Drury, K, Dulawan, P, Dunleavy, A, Dunn, S, Dupont, C, Earley, J, Easom, N, Echevarria, C, Edwards, S, Edwardson, C, El-Taweel, H, Elliott, A, Elliott, K, Ellis, Y, Elmer, A, Evans, D, Evans, H, Evans, J, Evans, R, Evans, R I, Evans, T, Evenden, C, Evison, L, Fabbri, L, Fairbairn, S, Fairman, A, Fallon, K, Faluyi, D, Favager, C, Fayzan, T, Featherstone, J, Felton, T, Finch, J, Finney, S, Finnigan, J, Finnigan, L, Fisher, H, Fletcher, S, Flockton, R, Flynn, M, Foot, H, Foote, D, Ford, A, Forton, D, Fraile, E, Francis, C, Francis, R, Francis, S, Frankel, A, Fraser, E, Free, R, French, N, Fu, X, Fuld, J, Furniss, J, Garner, L, Gautam, N, Geddes, J R, George, J, George, P M, Gibbons, M, Gill, M, Gilmour, L, Gleeson, F, Glossop, J, Glover, S, Goodman, N, Goodwin, C, Gooptu, B, Gordon, H, Gorsuch, T, Greatorex, M, Greenhaff, P L, Greenhalf, W, Greenhalgh, A, Greenwood, J, Gregory, H, Gregory, R, Grieve, D, Griffin, D, Griffiths, L, Guerdette, A-M, Guillen Guio, B, Gummadi, M, Gupta, A, Gurram, S, Guthrie, E, Guy, Z, Henson, H, Hadley, K, Haggar, A, Hainey, K, Hairsine, B, Haldar, P, Hall, I, Hall, L, Halling-Brown, M, Hamil, R, Hancock, A, Hancock, K, Haq, S, Hardwick, H E, Hardy, E, Hardy, T, Hargadon, B, Harrington, K, Harris, E, Harrison, P, Hart, N, Harvey, A, Harvey, M, Harvie, M, Haslam, L, Havinden-Williams, M, Hawkes, J, Hawkings, N, Haworth, J, Hayday, A, Haynes, M, Hazeldine, J, Hazelton, T, Heaney, L G, Heeley, C, Heeney, J L, Heightman, M, 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4. Clinical characteristics with inflammation profiling of long COVID and association with 1-year recovery following hospitalisation in the UK: a prospective observational study
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Evans, R A, Leavy, O C, Richardson, M, Elneima, O, McAuley, H J C, Shikotra, A, Singapuri, A, Sereno, M, Saunders, R M, Harris, V C, Houchen-Wolloff, L, Aul, R, Beirne, P, Bolton, C E, Brown, J S, Choudhury, G, Diar-Bakerly, N, Easom, N, Echevarria, C, Fuld, J, Hart, N, Hurst, J, Jones, M G, Parekh, D, Pfeffer, P, Rahman, N M, Rowland-Jones, S L, Shah, A M, Wootton, D G, Chalder, T, Davies, M J, De Soyza, A, Geddes, J R, Greenhalf, W, Greening, N J, Heaney, L G, Heller, S, Howard, L S, Jacob, J, Jenkins, R G, Lord, J M, Man, W D-C, McCann, G P, Neubauer, S, Openshaw, P J M, Porter, J C, Rowland, M J, Scott, J T, Semple, M G, Singh, S J, Thomas, D C, Toshner, M, Lewis, K E, Thwaites, R S, Briggs, A, Docherty, A B, Kerr, S, Lone, N I, Quint, J, Sheikh, A, Thorpe, M, Zheng, B, Chalmers, J D, Ho, L P, Horsley, A, Marks, M, Poinasamy, K, Raman, B, Harrison, E M, Wain, L V, Brightling, C E, Abel, K, Adamali, H, Adeloye, D, Adeyemi, O, Adrego, R, Aguilar Jimenez, L A, Ahmad, S, Ahmad Haider, 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Kurupati, P, Laing, C, Lamlum, H, Landers, G, Langenberg, C, Lasserson, D, Lavelle-Langham, L, Lawrie, A, Lawson, C, Layton, A, Lea, A, Lee, D, Lee, J-H, Lee, E, Leitch, K, Lenagh, R, Lewis, D, Lewis, J, Lewis, V, Lewis-Burke, N, Li, X, Light, T, Lightstone, L, Lilaonitkul, W, Lim, L, Linford, S, Lingford-Hughes, A, Lipman, M, Liyanage, K, Lloyd, A, Logan, S, Lomas, D, Loosley, R, Lota, H, Lovegrove, W, Lucey, A, Lukaschuk, E, Lye, A, Lynch, C, MacDonald, S, MacGowan, G, Macharia, I, Mackie, J, Macliver, L, Madathil, S, Madzamba, G, Magee, N, Magtoto, M M, Mairs, N, Majeed, N, Major, E, Malein, F, Malim, M, Mallison, G, Mandal, S, Mangion, K, Manisty, C, Manley, R, March, K, Marciniak, S, Marino, P, Mariveles, M, Marouzet, E, Marsh, S, Marshall, B, Marshall, M, Martin, J, Martineau, A, Martinez, L M, Maskell, N, Matila, D, Matimba-Mupaya, W, Matthews, L, Mbuyisa, A, McAdoo, S, Weir McCall, J, McAllister-Williams, H, McArdle, A, McArdle, P, McAulay, D, McCormick, J, McCormick, W, McCourt, P, McGarvey, L, McGee, C, Mcgee, K, McGinness, J, McGlynn, K, McGovern, A, McGuinness, H, McInnes, I B, McIntosh, J, McIvor, E, McIvor, K, McLeavey, L, McMahon, A, McMahon, M J, McMorrow, L, Mcnally, T, McNarry, M, McNeill, J, McQueen, A, McShane, H, Mears, C, Megson, C, Megson, S, Mehta, P, Meiring, J, Melling, L, Mencias, M, Menzies, D, Merida Morillas, M, Michael, A, Milligan, L, Miller, C, Mills, C, Mills, N L, Milner, L, Misra, S, Mitchell, J, Mohamed, A, Mohamed, N, Mohammed, S, Molyneaux, P L, Monteiro, W, Moriera, S, Morley, A, Morrison, L, Morriss, R, Morrow, A, Moss, A J, Moss, P, Motohashi, K, Msimanga, N, Mukaetova-Ladinska, E, Munawar, U, Murira, J, Nanda, U, Nassa, H, Nasseri, M, Neal, A, Needham, R, Neill, P, Newell, H, Newman, T, Newton-Cox, A, Nicholson, T, Nicoll, D, Nolan, C M, Noonan, M J, Norman, C, Novotny, P, Nunag, J, Nwafor, L, Nwanguma, U, Nyaboko, J, O'Donnell, K, O'Brien, C, O'Brien, L, O'Regan, D, Odell, N, Ogg, G, Olaosebikan, O, Oliver, C, Omar, Z, Orriss-Dib, L, Osborne, L, Osbourne, R, Ostermann, M, Overton, C, Owen, J, Oxton, J, Pack, J, Pacpaco, E, Paddick, S, Painter, S, Pakzad, A, Palmer, S, Papineni, P, Paques, K, Paradowski, K, Pareek, M, Parfrey, H, Pariante, C, Parker, S, Parkes, M, Parmar, J, Patale, S, Patel, B, Patel, M, Patel, S, Pattenadk, D, Pavlides, M, Payne, S, Pearce, L, Pearl, J E, Peckham, D, Pendlebury, J, Peng, Y, Pennington, C, Peralta, I, Perkins, E, Peterkin, Z, Peto, T, Petousi, N, Petrie, J, Phipps, J, Pimm, J, Piper Hanley, K, Pius, R, Plant, H, Plein, S, Plekhanova, T, Plowright, M, Polgar, O, Poll, L, Porter, J, Portukhay, S, Powell, N, Prabhu, A, Pratt, J, Price, A, Price, C, Price, D, Price, L, Prickett, A, Propescu, J, Pugmire, S, Quaid, S, Quigley, J, Qureshi, H, Qureshi, I N, Radhakrishnan, K, Ralser, M, Ramos, A, Ramos, H, Rangeley, J, Rangelov, B, Ratcliffe, L, Ravencroft, P, Reddington, A, Reddy, R, Redfearn, H, Redwood, D, Reed, A, Rees, M, Rees, T, Regan, K, Reynolds, W, Ribeiro, C, Richards, A, Richardson, E, Rivera-Ortega, P, Roberts, K, Robertson, E, Robinson, E, Robinson, L, Roche, L, Roddis, C, Rodger, J, Ross, A, Ross, G, Rossdale, J, Rostron, A, Rowe, A, Rowland, A, Rowland, J, Roy, K, Roy, M, Rudan, I, Russell, R, Russell, E, Saalmink, G, Sabit, R, Sage, E K, Samakomva, T, Samani, N, Sampson, C, Samuel, K, Samuel, R, Sanderson, A, Sapey, E, Saralaya, D, Sargant, J, Sarginson, C, Sass, T, Sattar, N, Saunders, K, Saunders, P, Saunders, L C, Savill, H, Saxon, W, Sayer, A, Schronce, J, Schwaeble, W, Scott, K, Selby, N, Sewell, T A, Shah, K, Shah, P, Shankar-Hari, M, Sharma, M, Sharpe, C, Sharpe, M, Shashaa, S, Shaw, A, Shaw, K, Shaw, V, Shelton, S, Shenton, L, Shevket, K, Short, J, Siddique, S, Siddiqui, S, Sidebottom, J, Sigfrid, L, Simons, G, Simpson, J, Simpson, N, Singh, C, Singh, S, Sissons, D, Skeemer, J, Slack, K, Smith, A, Smith, D, Smith, S, Smith, J, Smith, L, Soares, M, Solano, T S, Solly, R, Solstice, AR, Soulsby, T, Southern, D, Sowter, D, Spears, M, Spencer, L G, Speranza, F, Stadon, L, Stanel, S, Steele, N, Steiner, M, Stensel, D, Stephens, G, Stephenson, L, Stern, M, Stewart, I, Stimpson, R, Stockdale, S, Stockley, J, Stoker, W, Stone, R, Storrar, W, Storrie, A, Storton, K, Stringer, E, Strong-Sheldrake, S, Stroud, N, Subbe, C, Sudlow, C L, Suleiman, Z, Summers, C, Summersgill, C, Sutherland, D, Sykes, D L, Sykes, R, Talbot, N, Tan, A L, Tarusan, L, Tavoukjian, V, Taylor, A, Taylor, C, Taylor, J, Te, A, Tedd, H, Tee, CJ, Teixeira, J, Tench, H, Terry, S, Thackray-Nocera, S, Thaivalappil, F, Thamu, B, Thickett, D, Thomas, C, Thomas, S, Thomas, A K, Thomas-Woods, T, Thompson, T, Thompson, A A R, Thornton, T, Tilley, J, Tinker, N, Tiongson, G F, Tobin, M, Tomlinson, J, Tong, C, Touyz, R, Tripp, K A, Tunnicliffe, E, Turnbull, A, Turner, E, Turner, S, Turner, V, Turner, K, Turney, S, Turtle, L, Turton, H, Ugoji, J, Ugwuoke, R, Upthegrove, R, Valabhji, J, Ventura, M, Vere, J, Vickers, C, Vinson, B, Wade, E, Wade, P, Wainwright, T, Wajero, L O, Walder, S, Walker, S, Wall, E, Wallis, T, Walmsley, S, Walsh, J A, Walsh, S, Warburton, L, Ward, T J C, Warwick, K, Wassall, H, Waterson, S, Watson, E, Watson, L, Watson, J, Welch, C, Welch, H, Welsh, B, Wessely, S, West, S, Weston, H, Wheeler, H, White, S, Whitehead, V, Whitney, J, Whittaker, S, Whittam, B, Whitworth, V, Wight, A, Wild, J, Wilkins, M, Wilkinson, D, Williams, N, Williams, J, Williams-Howard, S A, Willicombe, M, Willis, G, Willoughby, J, Wilson, A, Wilson, D, Wilson, I, Window, N, Witham, M, Wolf-Roberts, R, Wood, C, Woodhead, F, Woods, J, Wormleighton, J, Worsley, J, Wraith, D, Wrey Brown, C, Wright, C, Wright, L, Wright, S, Wyles, J, Wynter, I, Xu, M, Yasmin, N, Yasmin, S, Yates, T, Yip, K P, Young, B, Young, S, Young, A, Yousuf, A J, Zawia, A, Zeidan, L, Zhao, B, and Zongo, O
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- 2022
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5. The Shape of Dark Matter Haloes III. Kinematics and Structure of the HI disc
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Peters, S. P. C., van der Kruit, P. C., Allen, R. J., and Freeman, K. C.
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Astrophysics - Astrophysics of Galaxies - Abstract
We present a new strategy for fitting the structure and kinematics of the HI in edge-on galaxies using a fit to the terminal-velocity channel maps of a HI data cube. The strategy can deal with self-absorbing HI gas and the presence of warps. The method is first tested on a series of models. We demonstrate that fitting optically thin models to real galaxies will lead to an overestimation of the thickness and velocity dispersion, and to a serious underestimation of the HI face-on column densities. We subsequently fit both self-absorption and optically thin models to the HI data of six edge-on galaxies. In three of these we have also measured the velocity dispersion. On average 27 \pm 6 % of the total HI mass of edge-on galaxies is hidden by self-absorption. This implies that the HI mass, thickness and velocity dispersion of galaxies is typically underestimated in the literature., Comment: Accepted for publication by Monthly Notices RAS. Hi-res. version available at www.astro.rug.nl/~vdkruit/Petersetal-III.pdf
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- 2016
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6. The Shape of Dark Matter Haloes II. The Galactus HI Modelling & Fitting Tool
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Peters, S. P. C., van der Kruit, P. C., Allen, R. J., and Freeman, K. C.
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Astrophysics - Astrophysics of Galaxies - Abstract
We present a new HI modelling tool called \textsc{Galactus}. The program has been designed to perform automated fits of disc-galaxy models to observations. It includes a treatment for the self-absorption of the gas. The software has been released into the public domain. We describe the design philosophy and inner workings of the program. After this, we model the face-on galaxy NGC2403, using both self-absorption and optically thin models, showing that self-absorption occurs even in face-on galaxies. It is shown that the maximum surface brightness plateaus seen in Paper I of this series are indeed signs of self-absorption. The apparent HI mass of an edge-on galaxy can be drastically lower compared to that same galaxy seen face-on. The Tully-Fisher relation is found to be relatively free from self-absorption issues., Comment: Accepted for publication by Monthly Notices RAS. Hi-res. version available at www.astro.rug.nl/~vdkruit/Petersetal-II.pdf
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- 2016
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7. The Shape of Dark Matter Haloes, V. Analysis of observations of edge-on galaxies
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Peters, S. P. C., van der Kruit, P. C., Allen, R. J., and Freeman, K. C.
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Astrophysics - Astrophysics of Galaxies - Abstract
In the previous papers in this series, we have measured the stellar and \hi content in a sample of edge-on galaxies. In the present paper, we perform a simultaneous rotation curve and vertical force field gradient decomposition for five of these edge-on galaxies. The rotation curve decomposition provides a measure of the radial dark matter potential, while the vertical force field gradient provide a measure of the vertical dark matter potential. We fit dark matter halo models to these potentials. Using our \hi self-absorption results, we find that a typical dark matter halo has a less dense core ($0.094\pm0.230$\,M$_\odot$/pc$^3$) compared to an optically thin \hi model ($0.150\pm0.124$\,M$_\odot$/pc$^3$). The HI self-absorption dark matter halo has a longer scale length $R_c$ of $1.42\pm 3.48$\,kpc, versus $1.10\pm 1.81$\,kpc for the optically thin HI model. The median halo shape is spherical, at $q=1.0\pm0.6$ (self-absorbing \hi), while it is prolate at $q=1.5\pm0.6$ for the optically thin. Our best results were obtained for ESO\,274-G001 and UGC\,7321, for which we were able to measure the velocity dispersion in Paper III. These two galaxies have drastically different halo shapes, with one oblate and one strongly prolate. Overall, we find that the many assumptions required make this type of analysis susceptible to errors., Comment: Accepted for publication by MNRAS. Earlier papers in the series are in the refereeing process. High-res. version of this paper is available at www.astro.rug.nl/~vdkruit/Petersetal-V.pdf
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- 2016
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8. A likely increase in fine particulate matter and premature mortality under future climate change
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Park, S., Allen, R. J., and Lim, C. H.
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- 2020
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9. The Shape of Dark Matter Haloes, I. HI Observations of Edge-on Galaxies
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Peters, S. P. C., van der Kruit, P. C., Allen, R. J., and Freeman, K. C.
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Astrophysics - Astrophysics of Galaxies ,Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
We present neutral hydrogen observations for a sample of eight nearby, late-type, edge-on galaxies. All of the galaxies have been well resolved in the radial direction, while six have also been well resolved in the vertical direction. We find that each of the galaxies has approximately the same maximum surface brightness temperature throughout its disc. We argue that self-absorption is the main cause of this phenomenon and that subsequent decompositions will require a treatment of this., Comment: Accepted for publication by MNRAS. High-res. version of this paper is available at www.astro.rug.nl/~vdkruit/Petersetal-I.pdf
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- 2013
10. The Opacity of Spiral Galaxy Disks IX; Dust and Gas Surface Densities
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Holwerda, B. W., Allen, R. J., de Blok, W. J. G., Bouchard, A., Gonzalez-Lopezlira, R. A., van der Kruit, P. C., and Leroy, A.
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Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
Our aim is to explore the relation between gas, atomic and molecular, and dust in spiral galaxies. Gas surface densities are from atomic hydrogen and CO line emission maps. To estimate the dust content, we use the disk opacity as inferred from the number of distant galaxies identified in twelve HST/WFPC2 fields of ten nearby spiral galaxies. The observed number of distant galaxies is calibrated for source confusion and crowding with artificial galaxy counts and here we verify our results with sub-mm surface brightnesses from archival Herschel-SPIRE data. We find that the opacity of the spiral disk does not correlate well with the surface density of atomic (Hi) or molecular hydrogen (H2) alone implying that dust is not only associated with the molecular clouds but also the diffuse atomic disk in these galaxies. Our result is a typical dust-to-gas ratio of 0.04, with some evidence that this ratio declines with galactocentric radius, consistent with recent Herschel results. We discuss the possible causes of this high dust-to-gas ratio; an over-estimate of the dust surface-density, an under-estimate of the molecular hydrogen density from CO maps or a combination of both. We note that while our value of the mean dust-to-gas ratio is high, it is consistent with the metallicity at the measured radii if one assumes the Pilyugin & Thuan calibration of gas metallicity., Comment: Accepted by AN, 15 pages, 10 figures, 1 table
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- 2012
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11. Evolution in the Dust Lane Fraction of Edge-on L* Spiral Galaxies since z=0.8
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Holwerda, B. W., Dalcanton, J. J., Radburn-Smith, D., de Jong, R. S., Guhathakurta, P., Koekemoer, A., Allen, R. J., and Böker, T.
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Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
The presence of a well-defined and narrow dust lane in an edge-on spiral galaxy is the observational signature of a thin and dense molecular disk, in which gravitational collapse has overcome turbulence. Using a sample of galaxies out to z~1 extracted from the COSMOS survey, we identify the fraction of massive disks that display a dust lane. Our goal is to explore the evolution in the stability of the molecular ISM disks in spiral galaxies over a cosmic timescale. We check the reliability of our morphological classifications against changes in restframe wavelength, resolution, and cosmic dimming with (artificially redshifted) images of local galaxies from SDSS. We find that the fraction of L* disks with dust lanes in COSMOS is consistent with the local fraction (~80%) out to z~0.7. At z=0.8, the dust lane fraction is only slightly lower. A somewhat lower dust lane fraction in starbursting galaxies tentatively supports the notion that a high specific star formation rate can efficiently destroy or inhibit a dense molecular disk. A small subsample of higher redshift COSMOS galaxies display low internal reddening (E[B-V]), as well as a low incidence of dust lanes. These may be disks in which the growth of the dusty ISM disk lags behind that of the stellar disk. We note that at z=0.8, the most massive galaxies display a lower dust lane fraction than lower mass galaxies. A small contribution of recent mergers or starbursts to this most massive population may be responsible. The fact that the fraction of galaxies with dust lanes in COSMOS is consistent with little or no evolution implies that models to explain the Spectral Energy Distribution or the host galaxy dust extinction of supernovae based on local galaxies are still applicable to higher redshift spirals. It also suggests that dust lanes are long lived phenomena or can be reformed over very short time-scales., Comment: 14 pages, 9 figures, 2 tables, accepted for publication by ApJ
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- 2012
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12. Five Supernova Survey Galaxies in the Southern Hemisphere: Supernova Ia Rates
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Hakobyan, A. A., Petrosian, A. R., Mamon, G. A., McLean, B., Kunth, D., Turatto, M., Cappellaro, E., Mannucci, F., Allen, R. J., Panagia, N., Della Valle, M., and Petrosyan, G. V.
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Astrophysics - Cosmology and Extragalactic Astrophysics - Abstract
Based on the database of 56 supernovae (SNe) events discovered in 3838 galaxies of the southern hemisphere, we compute the rate of SNe of different types along the Hubble sequence normalized to the optical and near-infrared (NIR) luminosities as well as to the stellar mass of the galaxies. We find that the rates of Type Ia SNe show a dependence on both morphology and colors of the galaxies, and therefore, on the star-formation activity. The rate of SNe Ia can be explained by assuming that at least 15% of Ia events in spiral galaxies originate in relatively young stellar populations. We also find that the rates show no modulation with nuclear activity or environment., Comment: 2 pages
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- 2011
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13. Five supernova survey galaxies in the southern hemisphere. II. The supernova rates
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Hakobyan, A. A., Petrosian, A. R., Mamon, G. A., McLean, B., Kunth, D., Turatto, M., Cappellaro, E., Mannucci, F., Allen, R. J., Panagia, N., and Della Valle, M.
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Astrophysics - Cosmology and Extragalactic Astrophysics - Abstract
Based on the database compiled in the first article of this series, with 56 SN events discovered in 3838 galaxies of the southern hemisphere, we compute the rate of supernovae (SNe) of different types along the Hubble sequence normalized to the optical and near-infrared luminosities as well as to the stellar mass of the galaxies. We find that the rates of all SN types show a dependence on both morphology and colors of the galaxies, and therefore, on the star-formation activity. The rate of core-collapse (CC) SNe is confirmed to be closely related to the Star Formation Rate (SFR) and only indirectly to the total mass of the galaxies. The rate of SNe Ia can be explained by assuming that at least 15% of Ia events in spiral galaxies originates in relatively young stellar populations. We find that the rates show no modulation with nuclear activity or environment. The ratio of SN rates between types Ib/c and II shows no trend with spiral type., Comment: 13 pages, 2 figures, 5 tables, published in Astrophysics (English translation of Astrofizika)
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- 2011
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14. The Second Byurakan Survey Galaxies. I. The Optical Database
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Gyulzadyan, M., Mclean, B., Adibekyan, V. Zh., Allen, R. J., Kunth, D., Petrosian, A., and Stepanian, J. A.
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Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
A database for the entire catalog of the Second Byurakan Survey (SBS) galaxies is presented. It contains new measurements of their optical parameters and additional information taken from the literature and other databases. The measurements were made using Ipg(near-infrared), Fpg(red) and Jpg(blue) band images from photographic sky survey plates obtained by the Palomar Schmidt telescope and extracted from the STScI Digital Sky Survey (DSS). The database provides accurate coordinates, morphological type, spectral and activity classes, apparent magnitudes and diameters, axial ratios, and position angles, as well as number counts of neighboring objects in a circle of radius 50 kpc. The total number of individual SBS objects in the database is now 1676. The 188 Markarian galaxies which were re-discovered by SBS are not included in this database. We also include redshifts that are now available for 1576 SBS objects, as well as 2MASS infrared magnitudes for 1117 SBS galaxies., Comment: 13 pages, 1 figure, 1 table
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- 2011
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15. Atomic Hydrogen produced in M33 Photodissociation Regions
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Heiner, J. S., Allen, R. J., and van der Kruit, P. C.
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Astrophysics - Astrophysics of Galaxies - Abstract
We derive total (atomic + molecular) hydrogen densities in giant molecular clouds (GMCs) in the nearby spiral galaxy M33 using a method that views the atomic hydrogen near regions of recent star formation as the product of photodissociation. Far-UV photons emanating from a nearby OB association produce a layer of atomic hydrogen on the surfaces of nearby GMCs. Our approach provides an estimate of the total hydrogen density in these GMCs from observations of the excess far-UV emission that reaches the GMC from the OB association, and the excess 21-cm radio HI emission produced after these far-UV photons convert H2 into HI on the GMC surface. The method provides an alternative approach to the use of CO emission as a tracer of H2 in GMCs, and is especially sensitive to a range of density well below the critical density for CO(1-0) emission. We describe our "PDR method" in more detail and apply it using GALEX far-UV and VLA 21-cm radio data to obtain volume densities in a selection of GMCs in the nearby spiral galaxy M33. We have also examined the sensitivity of the method to the linear resolution of the observations used; the results obtained at 20 pc are similar to those for the larger set of data at 80 pc resolution. The cloud densities we derive range from 1 to 500 cm-3, with no clear dependence on galactocentric radius; these results are generally similar to those obtained earlier in M81, M83, and M101 using the same method., Comment: Accepted for publication in MNRAS. 25 figures, 16 tables, including online-only materials
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- 2011
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16. The JCMT Nearby Galaxies Legacy Survey VI: The distribution of gas and star formation in M81
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Sánchez-Gallego, J. R., Knapen, J. H., Heiner, J. S., Wilson, C. D., Warren, B. E., Allen, R. J., Azimlu, M., Barmby, P., Bendo, G. J., Comerón, S., Israel, F. P., Serjeant, S., Tilanus, R. P. J., Vlahakis, C., and van der Werf, P.
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Astrophysics - Astrophysics of Galaxies - Abstract
We present a first complete 12 CO J=3-2 map of M81, observed as part of the Nearby Galaxies Legacy Survey being carried out at the James Clerk Maxwell Telescope. We detect 9 regions of significant CO emission located at different positions within the spiral arms, and confirm that the global CO emission in the galaxy is low. We combine these data with a new H-alpha map obtained using the Isaac Newton Telescope and archival HI, 24 microns and FUV images to uncover a correlation between the molecular gas and star forming regions in M81. For the nine regions detected in CO J=3-2, we combine our CO J=3-2 data with existing CO J=1-0 data to calculate line ratios. We find that the ratio J=(3-2)/(1-0) is in agreement with the range of typical values found in the literature (0.2-0.8). Making reasonable assumptions, this allows us to constrain the hydrogen density to the range (10^3-10^4) cm^{-3}. We also estimated the amount of hydrogen produced in photo-dissociation regions near the locations where CO J=3-2 was detected., Comment: Accepted for publication in Astronomy & Astrophysics. 11 pages, 4 figures
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- 2010
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17. A new method for obtaining the star formation law in galaxies
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Heiner, J. S., Allen, R. J., and van der Kruit, P. C.
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Astrophysics - Astrophysics of Galaxies - Abstract
We present a new observational method to evaluate the star formation law as formulated by Schmidt: the power-law expression assumed to relate the rate of star formation in a volume of space to the local total gas volume density. Volume densities in the clouds surrounding an OB association are determined with a simple model which considers atomic hydrogen as a photodissociation product on cloud surfaces. The photodissociating flux incident on the cloud is computed from the far-UV luminosity of the OB association and the geometry. We have applied this "PDR Method" to a sample of star-forming regions in M33 using VLA 21-cm data for the HI and GALEX imagery in the far-UV. It provides an estimate of the total volume density of hydrogen (atomic + molecular) in the gas clouds surrounding the young star cluster. A logarithmic graph of the cluster UV luminosity versus the surrounding gas density is a direct measure of the star formation law. However, this plot is severely affected by observational selection, rendering large areas of the diagram inaccessible to the data. An ordinary least-squares regression fit therefore gives a strongly biased result. Its slope primarily reflects the boundary defined when the 21-cm line becomes optically thick, no longer reliably measuring the HI column density. We use a maximum-likelihood statistical approach which can deal with truncated and skewed data, taking into account the large uncertainties in the derived total gas densities. The exponent we obtain for the Schmidt law in M33 is 1.4 \pm 0.2., Comment: Accepted for publication in ApJ
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- 2010
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18. Non-equilibrium dynamics of an active colloidal 'chucker'
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Valeriani, C., Allen, R. J., and Marenduzzo, D.
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Condensed Matter - Soft Condensed Matter - Abstract
We report Monte Carlo simulations of the dynamics of a "chucker": a colloidal particle which emits smaller solute particles from its surface, isotropically and at a constant rate k_c. We find that the diffusion constant of the chucker increases for small k_c, as recently predicted theoretically. At large k_c the chucker diffuses more slowly due to crowding effects. We compare our simulation results to those of a "point particle" Langevin dynamics scheme in which the solute concentration field is calculated analytically, and in which hydrodynamic effects can be included albeit in an approximate way. By simulating the dragging of a chucker, we obtain an estimate of its apparent mobility coefficient which violates the fluctuation-dissipation theorem. We also characterise the probability density profile for a chucker which sediments onto a surface which either repels or absorbs the solute particles, and find that the steady state distributions are very different in the two cases. Our simulations are inspired by the biological example of exopolysaccharide-producing bacteria, as well as by recent experimental, simulation and theoretical work on phoretic colloidal "swimmers"., Comment: re-submission after referee's comments
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- 2010
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19. A catalog of Kazarian galaxies
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Kazarian, M. A., Adibekyan, V. Zh., McLean, B., Allen, R. J., and Petrosian, A. R.
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Astrophysics - Cosmology and Nongalactic Astrophysics - Abstract
The entire Kazarian galaxies (KG) catalog is presented which combines extensive new measurements of their optical parameters with a literature and database search. The measurements were made using images extracted from the STScI Digitized Sky Survey (DSS) of Jpg(blue), Fpg(red) and Ipg(NIR) band photographic sky survey plates obtained by the Palomar and UK Schmidt telescopes. We provide accurate coordinates, morphological type, spectral and activity classes, blue apparent diameters, axial ratios, position angles, red, blue and NIR apparent magnitudes, as well as counts of neighboring objects in a circle of radius 50 kpc from centers of KG. Special attention was paid to the individual descriptions of the galaxies in the original Kazarian lists, which clarified many cases of misidentifications of the objects, particularly among interacting systems. The total number of individual Kazarian objects in the database is now 706. We also include the redshifts which are now available for 404 galaxies and the 2MASS infrared magnitudes for 598 KG. The database also includes extensive notes, which summarize information about the membership of KG in different systems of galaxies, and about revised activity classes and redshifts. An atlas of several interesting subclasses of KG is also presented., Comment: 15 pages, 5 figures, 1 table, Accepted in Astrophysics, Vol. 53, No. 1, 2010 (English translation of Astrofizika)
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- 2009
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20. A photodissociation model for the morphology of the HI near OB associations in M33
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Heiner, J. S., Allen, R. J., and van der Kruit, P. C.
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Astrophysics - Cosmology and Extragalactic Astrophysics - Abstract
We present an approach for analysing the morphology and physical properties of Hi features near giant OB asso- ciations in M33, in the context of a model whereby the Hi excess arises from photodissociation of the molecular gas in remnants of the parent Giant Molecular Clouds (GMCs). Examples are presented here in the environs of NGC604 and CPSDPZ204, two prominent Hii regions in M33. These are the first results of a detailed analysis of the environs of a large number of OB associations in that galaxy. We present evidence for "diffusion" of the far-UV radiation from the OB association through a clumpy remnant GMC, and show further that enhanced CO(1-0) emission appears preferentially associated with GMCs of higher volume density., Comment: Accepted to ApJ
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- 2009
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21. Five supernova survey galaxies in the southern hemisphere. I. Optical and near-infrared database
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Hakobyan, A. A., Petrosian, A. R., Mamon, G. A., McLean, B., Kunth, D., Turatto, M., Cappellaro, E., Mannucci, F., Allen, R. J., Panagia, N., and Della Valle, M.
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Astrophysics - Cosmology and Extragalactic Astrophysics - Abstract
The determination of the supernova (SN) rate is based not only on the number of detected events, but also on the properties of the parent galaxy population. This is the first paper of a series aimed at obtaining new, refined, SN rates from a set of five SN surveys, by making use of a joint analysis of near-infrared (NIR) data. We describe the properties of the 3838 galaxies that were monitored for SNe events, including newly determined morphologies and their DENIS and POSS-II/UKST I, 2MASS and DENIS J and Ks and 2MASS H magnitudes. We have compared 2MASS, DENIS and POSS-II/UKST IJK magnitudes in order to find possible systematic photometric shifts in the measurements. The DENIS and POSS-II/UKST I band magnitudes show large discrepancies (mean absolute difference of 0.4 mag), mostly due to different spectral responses of the two instruments, with an important contribution (0.33 mag rms) from the large uncertainties in the photometric calibration of the POSS-II and UKST photographic plates. In the other wavebands, the limiting near infrared magnitude, morphology and inclination of the galaxies are the most influential factors which affect the determination of photometry of the galaxies. Nevertheless, no significant systematic differences have been found between of any pair of NIR magnitude measurements, except for a few percent of galaxies showing large discrepancies. This allows us to combine DENIS and 2MASS data for the J and Ks filters., Comment: 17 pages, 3 figures, 5 tables, published in Astrophysics, Vol. 52, No. 1, 2009 (English translation of Astrofizika)
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- 2009
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22. Long COVID research: an update from the PHOSP-COVID Scientific Summit
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Brightling, Christopher E, primary, Evans, Rachael A, additional, Singapuri, Amisha, additional, Smith, Nikki, additional, Wain, Louise V, additional, Brightling, C E, additional, Evans, R A, additional, Wain, L V, additional, Chalmers, J D, additional, Harris, V C, additional, Ho, L P, additional, Horsley, A, additional, Houchen-Wolloff, L, additional, Marks, M, additional, Raman, B, additional, Singapuri, A, additional, Barran, P, additional, Bingham, M, additional, Chilvers, E R, additional, Daynes, E, additional, Efstathiou, C M, additional, Elneima, O, additional, Guillen Guio, B, additional, Harrison, E M, additional, Jenkins, R G, additional, Liew, F, additional, Lone, N I, additional, Lord, J M, additional, McAuley, H J C, additional, McCann, G P, additional, Mitchell, J, additional, Plekhanova, T, additional, Russell, R J, additional, Saunders, R M, additional, Semple, M G, additional, Smith, N, additional, Trivedi, D, additional, Turtle, L, additional, Walker, S, additional, Abel, K, additional, Adamali, H, additional, Adeloye, D, additional, Adeyemi, O, additional, Adrego, R, additional, Aguilar Jimenez, L A, additional, Ahmad, S, additional, Ahmad Haider, N, additional, Ahmed, R, additional, Ahwireng, N, additional, Ainsworth, M, additional, Al-Sheklly, B, additional, Alamoudi, A, additional, Ali, M, additional, Aljaroof, M, additional, Allan, L, additional, Allen, R J, additional, Allerton, L, additional, Allsop, L, additional, Allt, AM, additional, Almeida, P, additional, Altmann, D, additional, Alvarez Corral, M, additional, Amoils, S, additional, Anderson, D, additional, Antoniades, C, additional, Arbane, G, additional, Arias, A, additional, Armour, C, additional, Armstrong, L, additional, Armstrong, N, additional, Arnold, D, additional, Arnold, H, additional, Ashish, A, additional, Ashworth, A, additional, Ashworth, M, additional, Aslani, S, additional, Assefa-Kebede, H, additional, Atkin, P, additional, Atkin, C, additional, Aul, R, additional, Aung, H, additional, Austin, L, additional, Avram, C, additional, Ayoub, A, additional, Babores, M, additional, Baggott, R, additional, Bagshaw, J, additional, Baguley, D, additional, Bailey, L, additional, Baillie, J K, additional, Bain, S, additional, Bakali, M, additional, Bakau, M, additional, Baldry, E, additional, Baldwin, M, additional, Baldwin, D, additional, Ballard, C, additional, Banerjee, A, additional, Bang, D, additional, Barker, R E, additional, Barman, L, additional, Barratt, S, additional, Barrett, F, additional, Basire, D, additional, Basu, N, additional, Bates, M, additional, Bates, A, additional, Batterham, R, additional, Baxendale, H, additional, Baxter, G, additional, Bayes, H, additional, Beadsworth, M, additional, Beckett, P, additional, Beggs, M, additional, Begum, M, additional, Beirne, P, additional, Bell, M, additional, Bell, R, additional, Bennett, K, additional, Beranova, E, additional, Bermperi, A, additional, Berridge, A, additional, Berry, C, additional, Betts, S, additional, Bevan, E, additional, Bhui, K, additional, Birchall, K, additional, Bishop, L, additional, Bisnauthsing, K, additional, Blaikely, J, additional, Bloss, A, additional, Bolger, A, additional, Bolton, C E, additional, Bonnington, J, additional, Botkai, A, additional, Bourne, C, additional, Bourne, M, additional, Bramham, K, additional, Brear, L, additional, Breen, G, additional, Breeze, J, additional, Breeze, K, additional, Briggs, A, additional, Bright, E, additional, Brill, S, additional, Brindle, K, additional, Broad, L, additional, Broadley, A, additional, Brookes, C, additional, Broome, M, additional, Brown, V, additional, Brown, M, additional, Brown, J, additional, Brown, A, additional, Brown, J S, additional, Brugha, T, additional, Brunskill, N, additional, Buch, M, additional, Buckley, P, additional, Bularga, A, additional, Bullmore, E, additional, Bunker, J, additional, Burden, L, additional, Burdett, T, additional, Burn, D, additional, Burns, G, 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additional, Garner, L, additional, Gautam, N, additional, Geddes, J R, additional, George, J, additional, George, P, additional, Gibbons, M, additional, Gill, R, additional, Gill, M, additional, Gilmour, L, additional, Gleeson, F, additional, Glossop, J, additional, Glover, S, additional, Goodman, N, additional, Goodwin, C, additional, Gooptu, B, additional, Gordon, H, additional, Gorsuch, T, additional, Greatorex, M, additional, Greenhaff, P L, additional, Greenhalf, W, additional, Greenhalgh, A, additional, Greening, N J, additional, Greenwood, J, additional, Gregory, R, additional, Gregory, H, additional, Grieve, D, additional, Griffin, D, additional, Griffiths, L, additional, Guerdette, A-M, additional, Gummadi, M, additional, Gupta, A, additional, Gurram, S, additional, Guthrie, E, additional, Guy, Z, additional, Hadley, K, additional, Haggar, A, additional, Hainey, K, additional, Hairsine, B, additional, Haldar, P, additional, Hall, L, additional, Hall, I, additional, 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J, additional, Hogarth, P, additional, Holbourn, A, additional, Holden, S, additional, Holdsworth, L, additional, Holgate, D, additional, Holland, M, additional, Holloway, L, additional, Holmes, K, additional, Holmes, M, additional, Holroyd-Hind, B, additional, Holt, L, additional, Hormis, A, additional, Hosseini, A, additional, Hotopf, M, additional, Howard, L S, additional, Howard, K, additional, Howell, A, additional, Hufton, E, additional, Hughes, R A, additional, Hughes, J, additional, Hughes, A D, additional, Humphries, A, additional, Huneke, N, additional, Hurditch, E, additional, Hurst, J, additional, Husain, M, additional, Hussell, T, additional, Hutchinson, J, additional, Ibrahim, W, additional, Ilyas, F, additional, Ingham, J, additional, Ingram, L, additional, Ionita, D, additional, Isaacs, K, additional, Ismail, K, additional, Jackson, T, additional, Jacob, J, additional, James, W Y, additional, Jang, W, additional, Jarman, C, additional, Jarrold, I, additional, Jarvis, H, additional, Jastrub, R, additional, Jayaraman, B, additional, Jezzard, P, additional, Jiwa, K, additional, Johnson, C, additional, Johnson, S, additional, Johnston, D, additional, Jolley, C J, additional, Jones, S, additional, Jones, H, additional, Jones, L, additional, Jones, I, additional, Jones, G, additional, Jones, M G, additional, Jones, D, additional, Jose, S, additional, Kabir, T, additional, Kaltsakas, G, additional, Kamwa, V, additional, Kanellakis, N, additional, Kaprowska, S, additional, Kausar, Z, additional, Keenan, N, additional, Kelly, S, additional, Kemp, G, additional, Kerr, S, additional, Kerslake, H, additional, Key, A L, additional, Khan, F, additional, Khunti, K, additional, Kilroy, S, additional, King, B, additional, King, C, additional, Kingham, L, additional, Kirk, J, additional, Kitterick, P, additional, Klenerman, P, additional, Knibbs, L, additional, Knight, S, additional, Knighton, A, additional, Kon, O, additional, Kon, S, additional, Kon, S S, additional, Korszun, A, additional, Koychev, I, additional, Kurasz, C, additional, Kurupati, P, additional, Laing, C, additional, Lamlum, H, additional, Landers, G, additional, Langenberg, C, additional, Lavelle-Langham, L, additional, Lawrie, A, additional, Lawson, C, additional, Layton, A, additional, Lea, A, additional, Leavy, O C, additional, Lee, J-H, additional, Lee, E, additional, Lee, D, additional, Leitch, K, additional, Lenagh, R, additional, Lewis, V, additional, Lewis, J, additional, Lewis, K E, additional, Lewis, D, additional, Lewis-Burke, N, additional, Li, X, additional, Light, T, additional, Lightstone, L, additional, Lilaonitkul, W, additional, Lim, L, additional, Linford, S, additional, Lingford-Hughes, A, additional, Lipman, M, additional, Liyanage, K, additional, Lloyd, A, additional, Logan, S, additional, Lomas, D, additional, Loosley, R, additional, Lota, H, additional, Lovegrove, W, additional, Lucey, A, additional, Lucy, L, additional, Lukaschuk, E, additional, Lye, A, 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additional, Williams, B, additional, Williams, J, additional, Williams-Howard, S A, additional, Willicombe, M, additional, Willis, G, additional, Willoughby, J, additional, Wilson, A, additional, Wilson, I, additional, Wilson, D, additional, Window, N, additional, Witham, M, additional, Wolf-Roberts, R, additional, Wood, C, additional, Woodhead, F, additional, Woods, J, additional, Wootton, D G, additional, Wormleighton, J, additional, Worsley, J, additional, Wraith, D, additional, Wrey Brown, C, additional, Wright, C, additional, Wright, S, additional, Wright, L, additional, Wyles, J, additional, Wynter, I, additional, Xie, C, additional, Xu, M, additional, Yasmin, N, additional, Yasmin, S, additional, Yates, T, additional, Yip, K P, additional, Young, S, additional, Young, B, additional, Young, A, additional, Yousuf, A J, additional, Zawia, A, additional, Zeidan, L, additional, Zhao, B, additional, Zheng, B, additional, and Zongo, O, additional
- Published
- 2023
- Full Text
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23. Early-type galaxies with core collapse supernovae
- Author
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Hakobyan, A. A., Petrosian, A. R., McLean, B., Kunth, D., Allen, R. J., Turatto, M., and Barbon, R.
- Subjects
Astrophysics - Abstract
It is widely accepted that the progenitors of core collapse SNe are young massive stars and therefore their host galaxies are mostly spiral or irregular galaxies dominated by a young stellar population. Surprisingly, among morphologically classified hosts of core collapse SNe, we find 22 cases where the host has been classified as an Elliptical or S0 galaxy. To clarify this apparent contradiction, we carry out a detailed morphological study and an extensive literature search for additional information on the sample objects. Our results are as follows: 1. Of 22 "early type" objects, 17 are in fact misclassified spiral galaxies, one is a misclassified irregular, and one is a misclassified ring galaxy. 2. Of the 3 objects maintaining the early type classification, one (NGC2768) is a suspected merger remnant, another (NGC4589) is definitely a merger, and the third (NGC2274) is in close interaction. The presence of some amount of young stellar population in these galaxies is therefore not unexpected. These results confirm the presence of a limited, but significant, number of core collapse SNe in galaxies generally classified of early type. In all cases, anyway, there are independent indicators of the presence in host galaxies of recent star formation due to merging or gravitational interaction., Comment: 12 pages, 1 figure, 1 table, accepted for publication in A&A
- Published
- 2008
- Full Text
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24. Structure and Evolution of the Opacity of Spiral Disks
- Author
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Holwerda, B. W., Gonzalez, R. A., Keel, W. C., Calzetti, D., Allen, R. J., and van de Kruit, P. C.
- Subjects
Astrophysics - Abstract
The opacity of a spiral disk due to dust absorption influences every measurement we make of it in the UV and optical. Two separate techniques directly measure the total absorption by dust in the disk: calibrated distant galaxy counts and overlapping galaxy pairs. The main results from both so far are a semi-transparent disk with more opaque arms, and a relation between surface brightness and disk opacity. In the Spitzer era, SED models of spiral disks add a new perspective on the role of dust in spiral disks. Combined with the overall opacity from galaxy counts, they yield a typical optical depth of the dusty ISM clouds: 0.4 that implies a size of $\sim$ 60 pc. Work on galaxy counts is currently ongoing on the ACS fields of M51, M101 and M81. Occulting galaxies offer the possibility of probing the history of disk opacity from higher redshift pairs. Evolution in disk opacity could influence distance measurements (SN1a, Tully-Fisher relation). Here, we present first results from spectroscopically selected occulting pairs in the SDSS. The redshift range for this sample is limited, but does offer a first insight into disk opacity evolution as well as a reference for higher redshift measurements. Spiral disk opacity has not undergone significant evolution since z=0.2. HST imaging would help disentangle the effects of spiral arms in these pairs. Many more mixed-morphology types are being identified in SDSS by the GalaxyZoo project. The occulting galaxy technique can be pushed to a redshift of 1 using many pairs identified in the imaging campaigns with HST (DEEP2, GEMS, GOODS, COSMOS)., Comment: 8 pages, 4 figures, to appear in the proceedings of ``The Evolving ISM in the Milky Way and Nearby Galaxies'', Pasadena, 2007
- Published
- 2008
25. The Vertical Dust Structure in Spiral Disks
- Author
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Holwerda, B. W., Kamphuis, P., Allen, R. J., Peletier, R. F., and van der Kruit, P. C.
- Subjects
Astrophysics - Abstract
The halo of NGC 891 has been the subject of studies for more than a decade. One of its most striking features is the large asymmetry in H-$\alpha$ emission. We have taken a quantitative look at this asymmetry at different wavelengths for the first time. We propose that NGC 891 is intrinsically almost symmetric, as seen in Spitzer observations, and the large asymmetry in H-$\alpha$ emission is mostly due to dust attenuation. We quantify the additional optical depth needed to cause the observed H-$\alpha$ asymmetry. A comparison of large strips on the North East side of the galaxy with strips covering the same area in the South West we can quantify and analyze the asymmetry in the different wavelengths. From the 24 $\mu$m emission we find that the intrinsic asymmetry in star-formation in NGC 891 is small i.e., approximately 30%. The additional asymmetry in H-alpha is modeled as additional symmetric dust attenuation which extends up to ~ 40'' (1.9 kpc) above the plane of the galaxy with a mid-plane value of $\tau$=0.8 and a scale height of 0.5 kpc. This observational technique offers the possibility to quantify the effects of vertical ISM disk stability as an explanation for dust lanes in massive galaxies Dalcanton et al. (2004)., Comment: 4 pages, 3 figures, to appear in the proceedings of ``The Evolving ISM in the Milky Way and Nearby Galaxies'', Pasadena, 2007
- Published
- 2008
26. Eliminating fast reactions in stochastic simulations of biochemical networks: a bistable genetic switch
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Morelli, M. J., Allen, R. J., Tanase-Nicola, S., and Wolde, P. R. ten
- Subjects
Quantitative Biology - Quantitative Methods ,Quantitative Biology - Molecular Networks - Abstract
In many stochastic simulations of biochemical reaction networks, it is desirable to ``coarse-grain'' the reaction set, removing fast reactions while retaining the correct system dynamics. Various coarse-graining methods have been proposed, but it remains unclear which methods are reliable and which reactions can safely be eliminated. We address these issues for a model gene regulatory network that is particularly sensitive to dynamical fluctuations: a bistable genetic switch. We remove protein-DNA and/or protein-protein association-dissociation reactions from the reaction set, using various coarse-graining strategies. We determine the effects on the steady-state probability distribution function and on the rate of fluctuation-driven switch flipping transitions. We find that protein-protein interactions may be safely eliminated from the reaction set, but protein-DNA interactions may not. We also find that it is important to use the chemical master equation rather than macroscopic rate equations to compute effective propensity functions for the coarse-grained reactions., Comment: 46 pages, 5 figures
- Published
- 2007
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27. Reaction coordinates for the flipping of genetic switches
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Morelli, M. J., Tanase-Nicola, S., Allen, R. J., and Wolde, P. R. ten
- Subjects
Quantitative Biology - Molecular Networks ,Quantitative Biology - Quantitative Methods - Abstract
We present a detailed analysis, based on the Forward Flux Sampling (FFS) simulation method, of the switching dynamics and stability of two models of genetic toggle switches, consisting of two mutually-repressing genes encoding transcription factors (TFs); in one model (the exclusive switch), they mutually exclude each other's binding, while in the other model (general switch) the two transcription factors can bind simultaneously to the shared operator region. We assess the role of two pairs of reactions that influence the stability of these switches: TF-TF homodimerisation and TF-DNA association/dissociation. We factorise the flipping rate k into the product of the probability rho(q*) of finding the system at the dividing surface (separatrix) between the two stable states, and a kinetic prefactor R. In the case of the exclusive switch, the rate of TF-operator binding affects both rho(q*) and R, while the rate of TF dimerisation affects only R. In the case of the general switch both TF-operator binding and TF dimerisation affect k, R and rho(q*). To elucidate this, we analyse the transition state ensemble (TSE). For the exclusive switch, varying the rate of TF-operator binding can drastically change the pathway of switching, while changing the rate of dimerisation changes the switching rate without altering the mechanism. The switching pathways of the general switch are highly robust to changes in the rate constants of both TF-operator and TF-TF binding, even though these rate constants do affect the flipping rate; this feature is unique for non-equilibrium systems., Comment: 24 pages, 7 figures
- Published
- 2007
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28. Structure and Evolution of the Opacity of Spiral Disks
- Author
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Holwerda, B. W., González, R. A., Keel, W. C., Calzetti, D., Allen, R. J., and van de Kruit, P. C.
- Subjects
Astrophysics - Abstract
The opacity of a spiral disk due to dust absorption influences every measurement we make of it in the UV and optical. Two separate techniques directly measure the total absorption by dust in the disk: calibrated distant galaxy counts and overlapping galaxy pairs. The main results from both so far are a semi-transparent disk with more opaque arms, and a relation between surface brightness and disk opacity. In the Spitzer era, SED models of spiral disks add a new perspective on the role of dust in spiral disks. Combined with the overall opacity from galaxy counts, they yield a typical optical depth of the dusty ISM clouds: 0.4 that implies a size of ~60 pc. Work on galaxy counts is currently ongoing on the ACS fields of M51, M101 and M81. Occulting galaxies offer the possibility of probing the history of disk opacity from higher redshift pairs. Evolution in disk opacity could influence distance measurements (SN1a, Tully-Fisher relation). Here, we present first results from spectroscopically selected occulting pairs in the SDSS. The redshift range for this sample is limited, but does offer a first insight into disk opacity evolution as well as a reference for higher redshift measurements., Comment: 4 pages, 3 figures, to appear in the proceedings of "The Formation and Evolution of Galaxy Disks", Rome 2007, organized by the Vatican Observatory, editors J. G. Funes, S.J. and E. M. Corsini
- Published
- 2007
29. A dust component 2 kpc above the plane in NGC 891
- Author
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Kamphuis, P., Holwerda, B. W., Allen, R. J., Peletier, R. F., and van der Kruit, P. C.
- Subjects
Astrophysics - Abstract
The halo of NGC 891 has been the subject of studies for more than a decade. One of its most striking features is the large asymmetry in H$\alpha$ emission. In this letter, we will take a quantitative look at this asymmetry at different wavelengths for the first time. We suggest that NGC 891 is intrinsically almost symmetric and the large asymmetry in H$\alpha$ emission is mostly due to dust attenuation. We will quantify the additional optical depth needed to cause the observed asymmetry in this model. By comparing large strips on the North East side of the galaxy with strips covering the same area in the South West we can quantify and analyze the asymmetry in the different wavelengths. From the 24 $\mu$m emission we find that the intrinsic asymmetry in star formation in NGC 891 is small i.e., $\sim 30%$. The additional asymmetry in H$\alpha$ is modeled as additional symmetric dust attenuation which extends up to $\sim$ 40\arcsec (1.9 kpc) above the plane of the galaxy with a mid-plane value of $\tau$=0.8 and a scale height of 0.5 kpc, Comment: A&A in press. 5 pages, 3 figures
- Published
- 2007
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30. Kinematics of diffuse ionized gas in the disk halo interface of NGC 891 from Fabry-P\'erot observations
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Kamphuis, P., Peletier, R. F., Dettmar, R. -J., van der Hulst, J. M., van der Kruit, P. C., and Allen, R. J.
- Subjects
Astrophysics - Abstract
The properties of the gas in halos of galaxies constrain global models of the interstellar medium. Kinematical information is of particular interest since it is a clue to the origin of the gas. Here we report observations of the kinematics of the thick layer of the diffuse ionized gas in NGC 891 in order to determine the rotation curve of the halo gas. We have obtained a Fabry-P\'erot data cube in Halpha to measure the kinematics of the halo gas with angular resolution much higher than obtained from HI 21 cm observations. The data cube was obtained with the TAURUS II spectrograph at the WHT on La Palma. The velocity information of the diffuse ionized gas extracted from the data cube is compared to model distributions to constrain the distribution of the gas and in particular the halo rotation curve. The best fit model has a central attenuation tau_H-alpha=6, a dust scale length of 8.1 kpc, an ionized gas scale length of 5.0 kpc. Above the plane the rotation curve lags with a vertical gradient of -18.8 km/s/kpc. We find that the scale length of the H-alpha must be between 2.5 and 6.5 kpc. Furthermore we find evidence that the rotation curve above the plane rises less steeply than in the plane. This is all in agreement with the velocities measured in the HI., Comment: A&A, in press. 13 pages, 19 figures
- Published
- 2007
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31. CO emission from candidate photo-dissociation regions in M81
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Knapen, J. H., Allen, R. J., Heaton, H. I, Kuno, N., and Nakai, N.
- Subjects
Astrophysics - Abstract
Context At least a fraction of the atomic hydrogen in spiral galaxies is suspected to be the result of molecular hydrogen which has been dissociated by radiation from massive stars. Aims In this paper, we extend our earlier set of data from a small region of the Western spiral arm of M81 with CO observations in order to study the interplay between the radiation field and the molecular and atomic hydrogen. Methods We report CO(1-0) observations with the Nobeyama 45 m dish and the Owens Valley interferometer array of selected regions in the Western spiral arm of M81. Results From our Nobeyama data, we detect CO(1-0) emission at several locations, coinciding spatially with HI features near a far-UV source. The levels and widths of the detected CO profiles are consistent with the CO(1-0) emission that can be expected from several large photo-dissociation regions with typical sizes of some 50x150 pc located within our telescope beam. We do not detect emission at other pointings, even though several of those are near far-UV sources and accompanied by bright HI. This non-detection is likely a consequence of the marginal area filling factor of photo-dissociation regions in our observations. We detect no emission in our Owens Valley data, consistent with the low intensity of the CO emission detected in that field by the Nobeyama dish. Conclusions We explain the lack of CO(1-0) emission at positions farther from far-UV sources as a consequence of insufficient heating and excitation of the molecular gas at these positions, rather than as an absence of molecular hydrogen., Comment: 8 pages latex, 4 figures, Accepted for publication as a Research Note in Astronomy & Astrophysics
- Published
- 2006
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32. NGC922 - A new drop-through ring galaxy
- Author
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Wong, O. I., Meurer, G. R., Bekki, K., Hanish, D. J., Kennicutt, R. C., Bland-Hawthorn, J., Ryan-Weber, E. V., Koribalski, B., Kilborn, V. A., Putman, M. E., Heiner, J. S., Webster, R. L., Allen, R. J., Dopita, M. A., Doyle, M. T., Drinkwater, M. J., Ferguson, H. C., Freeman, K. C., Heckman, T. M., Hoopes, C., Knezek, P. M., Meyer, M. J., Oey, M. S., Seibert, M., Smith, R. C., Staveley-Smith, L., Thilker, D., Werk, J., and Zwaan, M. A.
- Subjects
Astrophysics - Abstract
We have found the peculiar galaxy NGC922 to be a new drop-through ring galaxy using multi-wavelength (UV-radio) imaging and spectroscopic observations. Its `C'-shaped morphology and tidal plume indicate a recent strong interaction with its companion which was identified with these observations. Using numerical simulations we demonstrate that the main properties of the system can be generated by a high-speed off-axis drop-through collision of a small galaxy with a larger disk system, thus making NGC922 one of the nearest known collisional ring galaxies. While these systems are rare in the local Universe, recent deep HST images suggest they were more common in the early Universe., Comment: 5 pages, accepted for publication in MNRAS Letters
- Published
- 2006
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33. Dust in spiral disks: opacity profiles from FIR emission and counts of distant galaxies
- Author
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Holwerda, B. W., Gonzalez, R. A., Calzetti, D., Allen, R. J., van der Kruit, P. C., and team, the SINGS
- Subjects
Astrophysics - Abstract
Dust emission in the far-infrared (FIR) characterizes the temperature and quantity of interstellar dust in a spiral disk. The three Spitzer/MIPS bands are well suited to measuring the gradient in temperature and the total optical depth in the disk of a spiral galaxy. Another way to estimate the quantity of dust in a spiral disk is the "Synthetic Field Method" (SFM, Gonzalez et al. 1998), which uses the number of distant field galaxies seen through the disk of the nearby spiral. The optical depth estimated from this method can be compared to the values derived from the FIR emission. Since the two techniques depend on different assumptions regarding the dust geometry and emissivity, this comparison between the optical depth profiles can potentially shed light on the structure and quantity of the ISM in spiral disks, especially any colder components. The dust responsible for the opacity from distant galaxy counts appears to be predominantly cold (T < 20 K.). The differences between the radial absorption profiles can be explained by spiral arms in the SFM measurements. Taken over the same aperture, galaxy counts show higher extinction values than the FIR derived ones. The implications for dust geometry can hopefully be explored with a more rigorous estimate of dust mass from the FIR fluxes., Comment: 4 pages, 4 figures to appear in the conference proceedings of "Infrared Diagnostics of Galaxy Evolution", Pasadena, 2005
- Published
- 2006
34. The Opacity of Spiral Galaxies from Counts of Distant Background Galaxies
- Author
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Holwerda, B. W., Gonzalez, R. A., Allen, R. J., and van der Kruit, P. C.
- Subjects
Astrophysics - Abstract
We have applied the "Synthetic Field Method" on a sample of ~20 nearby galaxies in order to determine the opacity of their disks. We present preliminary results on the radial dependence of cold dust absorption for 3 examples. The spirals NGC4535 and NGC4725 show significant absorption at a half-light radius. UGC2302, a LSB galaxy, shows much less opacity., Comment: 2 pages; Proceedings, Poster presented at IAU, Sidney, July 22, 2003
- Published
- 2003
35. Electric field-controlled water permeation coupled to ion transport through a nanopore
- Author
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Dzubiella, J., Allen, R. J., and Hansen, J. -P.
- Subjects
Physics - Biological Physics ,Physics - Chemical Physics - Abstract
We report Molecular Dynamics (MD) simulations of a generic hydrophobic nanopore connecting two reservoirs which are initially at different Na+ concentrations, as in a biological cell. The nanopore is impermeable to water under equilibrium conditions, but the strong electric field caused by the ionic concentration gradient drives water molecules in. The density and structure of water in the pore are highly field dependent. In a typical simulation run, we observe a succession of cation passages through the pore, characterized by approximately bulk mobility. These ion passages reduce the electric field, until the pore empties of water and closes to further ion transport, thus providing a possible mechanism for biological ion channel gating., Comment: 4 pages, 4 figures
- Published
- 2003
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36. Modelling the endothelial cell response to fluid flow
- Author
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Allen, R. J.
- Subjects
571.6 - Abstract
In vitro endothelial cells respond to fluid flow by elongating in the direction of flow. How the mechanical signal is transformed into an organised and directed response is poorly understood. The most studied and crucial aspects to this response are; actin filament alignment, mechano-transduction, signal transduction, Rho GTPase localised activation and lamellipodium formation. The goal of this project is to understand how these separate facets interact and lead to a coordinated response. The flow is modelled over a 3D virtual cell, which naturally gives the force the flow exerts on the cell surface via a boundary integral representation. This force is coupled to a Kelvin-body model of mechano-transduction which links, via a focal adhesion associated protein, Src, to a partial differential equation model (PDE) of the Rho GTPases Rac and Rho. The PDEs are integrated over a 2D projection of the 3D cell giving a time course for protein concentration at any point in the cell. It is demonstrated that a mechano-transducer that can respond to the normal component of the force is likely to be a necessary (though perhaps not sufficient) component of the signalling network. In some processes cross talk between the GTPases is thought to be important in forming spatially segregated zones of activation, for example in the front and back of migratory cells. This research shows that local signalling in endothelial cells could be initiated by the force normal to the surface of the cell and maintained by limited diffusion. Modelling indicates the EC signalling response to fluid flow may be attenuated by a change in morphology. Rac and Rho activation and deactivation are validated against experimentally reported time courses that have been taken for whole cell averages. However it will be demonstrated that these time courses do not characterise the process and therefore there is a need for more quantitative local measure of protein activation.
- Published
- 2009
37. The equilibrium response to idealized thermal forcings in a comprehensive GCM: implications for recent tropical expansion
- Author
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Allen, R. J, Sherwood, S. C, Norris, J. R, and Zender, C. S
- Subjects
Atmospheric circulation response ,tropopause height ,poleward shift ,black carbon ,climate ,perturbations ,reanalysis ,stratosphere ,variability ,troposphere - Abstract
Several recent studies have shown the width of the tropical belt has increased over the last several decades. The mechanisms driving tropical expansion are not well known and the recent expansion is underpredicted by state-of-the art GCMs. We use the CAM3 GCM to investigate how tropical width responds to idealized atmospheric heat sources, focusing on zonal displacement of the tropospheric jets. The heat sources include global and zonally restricted lower-tropospheric warmings and stratospheric coolings, which coarsely represent possible impacts of ozone or aerosol changes. Similar to prior studies with simplified GCMs, we find that stratospheric cooling - particularly at high-latitudes - shifts jets poleward and excites Northern and Southern Annular Mode (NAM/SAM)-type responses. We also find, however, that modest heating of the midlatitude boundary layer drives a similar response; heating at high latitudes provokes a weaker, equatorward shift and tropical heating produces no shift. Over 70 % of the variance in annual mean jet displacements across 27 experiments is accounted for by a newly proposed 'Expansion Index', which compares mid-latitude tropospheric warming to that at other latitudes. We find that previously proposed factors, including tropopause height and tropospheric stability, do not fully explain the results. Results suggest recently observed tropical expansion could have been driven not only by stratospheric cooling, but also by mid-latitude heating sources due for example to ozone or aerosol changes.
- Published
- 2012
38. The role of eastern Siberian snow and soil moisture anomalies in quasi-biennial persistence of the Arctic and North Atlantic Oscillations
- Author
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Allen, R. J and Zender, C. S
- Subjects
Southern oscillation ,geopotential height ,temperature-fields ,hemisphere winter ,stationary waves ,central Eurasia ,large-ensemble ,climate-change ,cover ,reanalysis - Abstract
Variations in the Arctic Oscillation (AO) and its regional manifestation, the North Atlantic Oscillation (NAO), generate much of the nonseasonal variability in the winter climate over the Northern Hemisphere midlatitudes. Despite being an internal mode of the atmosphere, the Arctic and North Atlantic Oscillations (N/AO) exhibit a slightly red spectrum, varying on quasi-biennial (2-3 years) and quasi-decadal time scales. Such low-frequency variability is likely due to the coupling of the atmosphere to boundary conditions and/or external forcings. Here we show that Eurasian snow cover, particularly over eastern Siberia (ESB), exhibits quasi-biennial persistence similar to the N/AO. Furthermore, the snow-AO mechanism operates on quasi-biennial timescales, with fall ESB snow cover significantly related to vertically propagating Rossby wave activity and the N/AO for the next two to three winters. On the basis of land surface model simulations from the Global Land Data Assimilation System (GLDAS), the interseasonal carryover of ESB snow is related to soil moisture anomalies and an evaporation-convection feedback. These findings suggest quasi-biennial persistence of the N/AO is partly due to land surface forcing in the form of both ESB snow and soil moisture anomalies.
- Published
- 2011
39. Imaging and Nulling with the Space Interferometry Mission
- Author
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Boeker, T. and Allen, R. J.
- Subjects
Astrophysics - Abstract
We present numerical simulations for a possible synthesis imaging mode of the Space Interferometer Mission (SIM). We summarize the general techniques that SIM offers to perform imaging of high surface brightness sources, and discuss their strengths and weaknesses. We describe an interactive software package that is used to provide realistic, photometrically correct estimates of SIM performance for various classes of astronomical objects. In particular, we simulate the cases of gaseous disks around black holes in the nuclei of galaxies, and zodiacal dust disks around young stellar objects. Regarding the first, we show that a Keplerian velocity gradient of the line-emitting gaseous disk -- and thus the mass of the putative black hole -- can be determined with SIM to unprecedented accuracy in about 5 hours of integration time for objects with H_alpha surface brigthness comparable to the prototype M 87. Detections and observations of exo-zodiacal dust disks depend critically on the disk properties and the nulling capabilities of SIM. Systems with similar disk size and at least one tenth of the dust content of beta Pic can be detected by SIM at distances between 100 pc and a few kpc, if a nulling efficiency of 1/10000 is achieved. Possible inner clear regions indicative of the presence of massive planets can also be detected and imaged. On the other hand, exo-zodiacal disks with properties more similar to the solar system will not be found in reasonable integration times with SIM., Comment: 28 pages, incl. 8 postscript figures, excl. 10 gif-figures Submitted to ApJ
- Published
- 1999
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40. Effects of continental-scale snow albedo anomalies on the wintertime Arctic oscillation
- Author
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Allen, R. J and Zender, C. S
- Subjects
snow cover ,Arctic Oscillation - Abstract
The NCAR CAM3 GCM with prescribed, satellite-based snow albedo (SA) is used to investigate the remote effects of snow cover on Northern Hemisphere (NH) winter climate. A pair of 100 ensemble member experiments are integrated through the autumn-winter season, with prescribed high and low SA over Eurasia (EA). Similar to other non-CAM GCM studies using prescribed snow mass, anomalous EA snow albedo produces a wave activity pulse that propagates into the stratosphere, culminating in a negative phase Arctic Oscillation– (AO-) like surface response. This occurs for idealized but representative SA anomalies, as well as for more realistic SA anomalies. Similar experiments over North America (NA) and the entire NH are also performed. Unlike prior studies, anomalous NA snow yields a significant AO signal. Here, the local NA surface cooling elicits a transient eddy response, which propagates downstream to Eurasia, resulting in significant but short-lived cooling and upward propagating wave activity over Siberia. A negative AO-like response develops, primarily confined to the stratosphere/upper troposphere, which eventually gives way to a tropospheric AO-like response of the opposite phase, due to equatorward wave refraction and wave divergence. Reanalysis data support this NA snow-positive AO response. Snow forcing experiments for the whole NH, however, yield a weakened AO signal. This is due to a muted wavenumber-1 and -2 response caused by destructive interference between the background stationary wave and the corresponding Rossby wave response, which results in negligible wave activity reaching the stratosphere.
- Published
- 2010
41. The Opacity of Nearby Galaxies from Colors and Counts of Background Galaxies: I. The Synthetic Field Method and its Application to NGC 4536 and NGC 3664
- Author
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Gonzalez, Rosa A., Allen, R. J., Dirsch, Boris, Ferguson, Harry C., Calzetti, Daniela, and Panagia, Nino
- Subjects
Astrophysics - Abstract
We describe a new, direct method for determining the opacity of foreground galaxies which does not require any a priori assumptions about the spatial distribution or the reddening law of the obscuring material. The method is to measure the colors and counts of background galaxies which can be identified through the foreground system. The method is calibrated, and the effects of confusion and obscuration are decoupled by adding various versions of a suitable deep reference frame containing only field galaxies with known properties into the image of the foreground galaxy, and analyzing these ``synthetic field'' images in the same way as the real images. We test the method on HST WFPC2 archived images of two galaxies which are quite different: NGC 4536 is a large Sc spiral, and NGC 3664 is a small Magellanic irregular. The reference frames are taken from the Hubble Deep Field. From the background galaxy counts, NGC 4536 shows an extinction A_I ~ 1 mag in the northwestern arm region, and lower than 0.5 mag in the corresponding interarm region (no correction for inclination has been attempted). However, from the galaxy colors, the same reddening of E(V - I) ~ 0.2 is observed in both the arm and the interarm regions. In the interarm region, the combination of extinction and reddening can be explained by a diffuse component with a Galactic reddening law (R_V ~ 3). In the spiral arm, however, the same diffuse, low opacity component seems to coexist with regions of much higher opacity. Since the exposures are shorter the results for NGC 3664 are less clear, but also appear to be consistent with a two component distribution., Comment: 42 pages, 18 figures; accepted for publication in The Astrophysical Journal, Vol. 506, October 10, 1998
- Published
- 1998
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42. Evidence for the Large-Scale Dissociation of Molecular Gas in the Inner Spiral Arms of M81
- Author
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Allen, R. J., Knapen, J. H., Bohlin, R., and Stecher, T.
- Subjects
Astrophysics - Abstract
We compare the detailed distributions of HI, H alpha, and 150 nm far-UV continuum emission in the spiral arms of M81 at a resolution of 9" (linear resolution 150 pc at 3.7 Mpc distance). The bright H alpha emission peaks are always associated with peaks in the far-UV emission. The converse is not always true; there are many regions of far-UV emission with little corresponding H alpha. The HI and the far-UV are always closely associated, in the sense that the HI is often brightest around the edges of the far-UV emission. The effects of extinction on the morphology are small, even in the far-UV. Extensive far-UV emission, often with little corresponding H alpha, indicates the presence of many ``B-stars'', which produce mostly non-ionizing UV photons. These far-UV photons dissociate a small fraction of an extensive layer of H_2 into HI. The observed morphology can be understood if ``chimneys'' are common in the spiral arms of M81, where holes are blown out of the galactic disk, exposing the bright HII regions and the corresponding far-UV associated with vigorous star formation. These ``naked'' star-forming regions show little obscuration. H_2 is turned into HI by UV photons impinging on the interior surfaces of these chimneys. The intensity of the far-UV radiation measured by UIT can dissociate the underlying H_2 with a typical density of ~10 H nucleii cm**-3 to produce the observed amount of HI in the spiral arms of M81. Except for thin surface layers locally heated in these photo-dissociation regions close to the far-UV sources, the bulk of the molecular gas in the inner disk of M81 is apparently too cold to produce much 12CO(1-0) emission., Comment: 12 pages, Latex. 8 postscript files. Better quality versions of the figures available from ftp://star.herts.ac.uk/pub/Knapen/m81uv . Accepted, ApJ
- Published
- 1997
- Full Text
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43. Classifying the unclassifiable—a Delphi study to reach consensus on the fibrotic nature of diseases
- Author
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Massen, G M, primary, Allen, R J, additional, Leavy, O C, additional, Selby, N M, additional, Aithal, G P, additional, Oliver, N, additional, Parfrey, H, additional, Wain, L V, additional, Jenkins, G, additional, Stewart, I, additional, and Quint, J K, additional
- Published
- 2023
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44. Single cell RNA sequencing suggests Gαi2 is associated with ILD in pigeon fanciers
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Somma, D, primary, Spears, M, additional, Wain, L V, additional, Allen, R J, additional, Leavy, O C, additional, Gooptu, B, additional, Bourke, S J, additional, Kurowska-Stolarska, M, additional, and Mcsharry, C, additional
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- 2022
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45. Binding in visual working memory
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Baddeley, A. D., primary, Allen, R. J., additional, and Hitch, G. J., additional
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- 2017
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46. Working Memory and Binding in Sentence Recall
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Baddeley, A. D., Hitch, G. J., and Allen, R. J.
- Abstract
A series of experiments explored whether chunking in short-term memory for verbal materials depends on attentionally limited executive processes. Secondary tasks were used to disrupt components of working memory and chunking was indexed by the sentence superiority effect, whereby immediate recall is better for sentences than word lists. To facilitate comparisons and maximise demands on working memory, materials were constrained by re-sampling a small set of words. Experiment 1 confirmed a reliable sentence superiority effect with constrained materials. Experiment 2 showed that secondary tasks of concurrent articulation and visual choice reaction impaired recall, but did not remove or reduce the sentence superiority effect. This was also the case with visual and verbal n-back concurrent tasks (Experiment 3), and with concurrent backward counting (Experiment 4). Backward counting did however interact with mode of presenting the memory materials, suggesting that our failure to find interactions between concurrent task and materials was not attributable to our methodology. We conclude that executive processes are not crucial for the sentence chunking advantage and we discuss implications for the episodic buffer and other theoretical accounts of working memory and chunking. (Contains 5 tables and 6 figures.)
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- 2009
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47. Leveraging global multi-ancestry meta-analysis in the study of idiopathic pulmonary fibrosis genetics
- Author
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Partanen, J. J. (Juulia J.), Häppölä, P. (Paavo), Zhou, W. (Wei), Lehisto, A. A. (Arto A.), Ainola, M. (Mari), Sutinen, E. (Eva), Allen, R. J. (Richard J.), Stockwell, A. D. (Amy D.), Leavy, O. C. (Olivia C.), Oldham, J. M. (Justin M.), Guillen-Guio, B. (Beatriz), Cox, N. J. (Nancy J.), Hirbo, J. B. (Jibril B.), Schwartz, D. A. (David A.), Fingerlin, T. E. (Tasha E.), Flores, C. (Carlos), Noth, I. (Imre), Yaspan, B. L. (Brian L.), Jenkins, R. G. (R. Gisli), Wain, L. V. (Louise V.), Ripatti, S. (Samuli), Pirinen, M. (Matti), I. I. (International IPF Genetics Consortium), G. B. (Global Biobank Meta-Analysis Initiative (GBMI)), Laitinen, T. (Tarja), Kaarteenaho, R. (Riitta), Myllärniemi, M. (Marjukka), Daly, M. J. (Mark J.), Koskela, J. T. (Jukka T.), Partanen, J. J. (Juulia J.), Häppölä, P. (Paavo), Zhou, W. (Wei), Lehisto, A. A. (Arto A.), Ainola, M. (Mari), Sutinen, E. (Eva), Allen, R. J. (Richard J.), Stockwell, A. D. (Amy D.), Leavy, O. C. (Olivia C.), Oldham, J. M. (Justin M.), Guillen-Guio, B. (Beatriz), Cox, N. J. (Nancy J.), Hirbo, J. B. (Jibril B.), Schwartz, D. A. (David A.), Fingerlin, T. E. (Tasha E.), Flores, C. (Carlos), Noth, I. (Imre), Yaspan, B. L. (Brian L.), Jenkins, R. G. (R. Gisli), Wain, L. V. (Louise V.), Ripatti, S. (Samuli), Pirinen, M. (Matti), I. I. (International IPF Genetics Consortium), G. B. (Global Biobank Meta-Analysis Initiative (GBMI)), Laitinen, T. (Tarja), Kaarteenaho, R. (Riitta), Myllärniemi, M. (Marjukka), Daly, M. J. (Mark J.), and Koskela, J. T. (Jukka T.)
- Abstract
Summary The research of rare and devastating orphan diseases, such as idiopathic pulmonary fibrosis (IPF) has been limited by the rarity of the disease itself. The prognosis is poor—the prevalence of IPF is only approximately four times the incidence, limiting the recruitment of patients to trials and studies of the underlying biology. Global biobanking efforts can dramatically alter the future of IPF research. We describe a large-scale meta-analysis of IPF, with 8,492 patients and 1,355,819 population controls from 13 biobanks around the globe. Finally, we combine this meta-analysis with the largest available meta-analysis of IPF, reaching 11,160 patients and 1,364,410 population controls. We identify seven novel genome-wide significant loci, only one of which would have been identified if the analysis had been limited to European ancestry individuals. We observe notable pleiotropy across IPF susceptibility and severe COVID-19 infection and note an unexplained sex-heterogeneity effect at the strongest IPF locus MUC5B.
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- 2022
48. The Fourier-Kelvin Stellar Interferometer: A Progress Report and Preliminary Results from our Laboratory Testbed
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Barry, R. K., Danchi, W. C., Rajagopal, J., Richardson, L. J., Kuchner, M., Wallace, D., Chambers, V. J., Martino, A., Traub, W., Ford, H., Allen, R. J., Seager, S., Leibundgut, Bruno, editor, Richichi, A., editor, Delplancke, F., editor, Paresce, F., editor, and Chelli, A., editor
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- 2008
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49. CO Emission from Massive Molecular Clouds in the Inner Disk of M31 : Optical Depths, Excitation Temperatures, and Densities
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Allen, R. J., Lequeux, J., Genzel, R., editor, and Harris, A. I., editor
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- 1994
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50. A catalog of Kazarian galaxies
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Kazarian, M. A., Adibekyan, V. Zh., McLean, B., Allen, R. J., and Petrosian, A. R.
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- 2010
- Full Text
- View/download PDF
Catalog
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