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Proposal Identification No.:

A2848 Arecibo Observatory

Date Received: 2013-Sep-03 07:58:15 William E. Gordon Telescope Observing Time Request COVER SHEET

Section I - General Information
Submitted for Sep 1 2013. This proposal has not been submitted before. Proposal Type: General Category: Sub-Category: Observation Category: Time Requested this semester: Hours already used for this pro ject: Additional Hours required to complete pro ject: Minimum Useful Time: Expected Data Storage: Prop osal Title: ABSTRACT: Regular Astronomy Spectroscopy Extragalactic 36 0 30 mins (5 on-source, 15 slew, 10 off/cal) less than 100 GB

HI in dusty early-type galaxies: probing the minor merger process

We propose an HI study of 13 nearby, massive early-type galaxies with prominent dust lanes, systems that are considered to be remnants of recent minor mergers between spheroidearly-type galaxies and gas-rich dwarfs. Combined with our existing UV to far-infrared analysis of these ob jects using GALEX, SDSS, UKIDSS, WISE and Herschel-ATLAS surveys, as well as the recently obtained IRAM CO data, we will be able to estimate: (1) the gas masses involved in minor mergers; (2) the gas-to-dust ratios of the accreted satellites; (3) star formation efficiencies in minor mergers; and (4) the breakdown between atomic and molecular gas in such interactions. HI characterisation is an important step in our aim to produce a detailed empirical description of the role of gas in the minor merger process, which is a significant driver of cosmic star formation and AGN activity at late epochs, but is currently poorly understood. Outreach Abstract: El telescopio mґ grande del mundo serґ usado para descubrir las ondas de radio mas dґ diles emitidas as a e por el gas atґ omico en galaxias que se encuentran a mas de mil millones de anos en el pasado. Las ~ galaxias que estudiamos son particularmente interesantes dado que cada una de ellas ha absorbido recientemente a alguna galaxia vecina mas pequena. El estudio de los efectos de estas interacciones entre ~ galaxias es vital porque se cree que la estructura completa del Universo se ha desarrollado a trave s de interacciones entre galaxias. Las observaciones que proponemos sera n usadas para determinar cuanto hidrґ ogeno atґ omico (el combustible para la formaciґ estelar) se encuentra en estas galaxias que han on colisionado y se han fusionado.

Name James R Allison Stanislav S Shabala

Institution University of Sydney University of Tasmania

E-mail jra@physics.usyd.edu.au stanislav.shabala@utas.edu.au

Phone +61 293518699 +61 362268502

Student no no

1

Additional Authors
Sugata Kavira j, skavira j@astro.ox.ac.uk Timothy Davis, tdavis@eso.org Kate Rowlands, kerowlands@googlemail.com Yuan-Sen Ting (Graduate Student), yuan-sen.ting@cfa.harvard.edu Catherine Vlahakis, cvlahaki@alma.cl Matthew Smith, matthew.smith@astro.cf.ac.uk Nicola Agius (Graduate Student), nkagius@uclan.ac.uk Pasquale Temi, pasquale.temi@nasa.gov Lulu Fan, fan@sissa.it Michal Michalowski, mm@roe.ac.uk Alexandre Amblard, alexandre.amblard@nasa.gov Maarten Baes, maarten.baes@ugent.be

This work is not part of a thesis.

Remote Observing Request

X

Observer will travel to AO Remote Observing In Absentia (instructions to operator)

Section I I - Time Request
The following times are in LST. For these observations night-time is not needed.

Begin End IntervalInterval 08:50 09:15 11:40 15:05

Days Needed at This Interval 2.5 11

Time Constraints (Must Be Justified in the Prop osal Text) Our time constraints are set by the visible LST range of the 13 galaxies in our sample, and the on-source integration time that is required to reach the pre-defined sensitivity limits. We give the visible LST range and the required on-source integration time for each galaxy in our sample in Fig. 3 and Table 1 of the proposal. We have no constraints on the calendar date, beyond those set by radio frequency interference. 2

Section I I I - Instruments Needed
L-wide Atmospheric Observation Instruments:

Sp ecial Equipment or setup:

none

Section IV - RFI Considerations Frequency Ranges Planned
1300-1400 1485-1685 This proposal requires Iridium RFI protection at 1612 MHz between 10pm and 6am EST. This proposal requires coordination with Punta Salinas radar within the band 1222-1381 MHz.. This proposal requires coordination with GPS L3 at 1381 MHz.

Section V - Observing List Target List
#Ob ject RA(J2000) Dec(J2000) Rise(LST) Set(LST) 2MASXJ09033081-0106127 09:03:30.8 -1:06:12.5 08:53:28 09:14:56 2MASXJ14161186+0152048 14:16:11.8 1:52:04.7 13:33:22 15:00:25 2MASXJ13341710+3455455 13:34:17.1 34:55:45.6 12:46:34 14:23:13 NGC5233 13:35:13.3 34:40:38.8 12:45:53 14:25:47 2MFGC10709 13:22:34.8 33:09:25.7 12:24:55 14:21:29 UGC08505 13:30:43.1 33:54:59.8 12:36:55 14:25:45 UGC08536 13:33:16.3 34:32:13.2 12:43:03 14:24:43 2MASXJ13411704+2616190 13:41:17.1 26:16:19.4 12:23:43 15:00:07 2MASXJ12581769+2708117 12:58:17.7 27:08:11.3 11:42:13 14:15:41 2MASXJ13010083+2701312 13:01:00.9 27:01:31.6 11:44:44 14:18:36 2MASXJ13333299+2616190 13:33:33.1 26:16:19.1 12:15:59 14:52:23 2MASXJ13244786+2417386 13:24:47.8 24:17:38.4 12:04:39 14:46:14 CGCG013-092 12:10:17.9 -00:31:04.4 11:49:12 12:32:47

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