Italian ARC - User contributions [en]

The ARC cluster

2023-01-26T14:49:17Z

Kazi: /* Computing Nodes */

The ARC is equipped with a dedicated computer server connected with a high-speed optical fiber network to the outside world, allowing fast data transfer (10 Gbit/sec).

Presently we have 200 Tb of diskspace and one 26 nodes cluster (112 cores) dedicated to the ARC.

ALMA and CASA users can request access to the server and the disk space by sending an e-mail to ''arc-support at ira.inaf.it'' indicating the reason for the request.

[[File:Blade.jpg|thumbnail]]

== User policy==

New ARC users can access the Italian ARC node computing facilities by requesting a face-2-face visit (ALMA users only, through the ALMA Helpdesk) or by visiting the ARC node in Bologna (for any data-reduction-related issue to be solved in collaboration with the ARC staff). In both the cases they are requested to send an e-mail to help-desk@alma.inaf.it indicating the reason for the request.

Please notice that the request for a new account for a new requesting user implies that he/she (and/or his/her collaborators) visits the ARC for an induction on the ARC facilities usage and on issues related to data reduction with CASA both for ALMA or any other telescope. If the request is positively evaluated the visit details will be arranged via e-mail.

The account will guarantee the usage of the facilities and the support for 6 months.

Once the account expires the access to the data will be suspended and, after 1 month of quarantine ALL DATA WILL BE REMOVED. Only one gentle reminder will be send on account expiration.
Extensions of the account duration period could be considered on request (via e-mail). No visit is needed in case of account renewal.

The ARC members support is guaranteed for any ALMA-related issue.
For data-reduction-related issues that do not involve ALMA, the support (other than the technical support in the usage of the ARC computing facilities) is limited to the knowledge/experience and availability of the ARC members.

The same rules apply also to IRA staff members. IRA collaborators with temporary positions (i.e. students) can have an account for the entire duration of their position.

To ensure a well-balanced load on the cluster nodes please follow instructions about accessing the computer cluster

Queries can be issued via e-mail to help-desk@alma.inaf.it

Users will be automatically added to the arc-cluster-users@ira.inaf.it mailing list that will be used for any communication from our side.

== Accessing the computer cluster ==

Once you have obtained an '''ARC''' account at '''IRA''', you can access the computer cluster nodes from everywhere through host '''scheduler.ira.inaf.it.'''.
Using graphical applications on the cluster is possible through remote X access.
The accessible working nodes are listed in the table below.
You can enter a node for interactive work by typing:

<source lang="bash">ssh -X ''<node>''.ira.inaf.it</source>

''Useful tip: by typing 'hostname' you can know on which node you are''

[http://ganglia.ira.inaf.it/?r=hour&cs=&ce=&c=unspecified&h=&tab=m&vn=&hide-hf=false&m=load_one&sh=1&z=small&hc=4&host_regex=%5Earc&max_graphs=0&s=by+name Here] you can find some statistics about resources consumption on the arcblXX nodes.

== Using ARC storage ==

You need to change directory to access your ARC storage on the cluster:

<source lang="bash"> cd /iranet/homesarc/''username'' </source>

On each node you can also use local disks on path /local/work/username (if allocated) and /local/scratch

/local/scratch will be emptied on every reboot

Beware that local disks have '''no redundancy at all''', never leave important data on them

=== Mounting ARC storage on you workstation ===

On IRA workstations ARC home filesystem can be accessed on ''/iranet/homesarc''

On your laptop ARC filesystems can be seamlessly accessed with fuse-sshfs:

as root, install the package sshfs

<source lang="bash">
# on RedHat/Centos/ScientificLinux
yum install fuse-sshfs

# on Debian/Ubuntu
apt-get install sshfs
</source>

then, as user

<source lang="bash">sshfs storage.alma.inaf.it:/iranet/homesarc/yourhome /your/local/mount/point/</source>

By omitting /remote/path you can mount you home directory.

Be aware that this method is suboptimal for heavy input/output loads. Running disk-intensive applications directly on the arc cluster will result in a file access speed 10-50 times faster.

== Software packages available ==

Software available on ARC cluster could be listed typing the command ''setup-help'' or on [https://www.ira.inaf.it/wiki/index.php/Arcsoft this page]

== Computing Nodes ==
{| class="wikitable"
|-
! Name !! RAM !! CPU !! Cores !! Clock !! Data Net !! Work Disk !! Scratch Disk !! scheduler !! groups !! notes
|-
|arcbl01||256G||Intel Xeon E5-1650 v4||6/12||3600||10GbE||15T||57G||N||arc-staff, arc-vlbi, arc-f2f||
|-
|arcbl17||64G||AMD Ryzen 7 1800X||8/16||3600||1GbE||3,5TB|| ||N||arc-staff, arc-vlbi||
|-
|arcbl18||64G||Intel Xeon E3-1275 v6||4/8||3800||10GbE||22T||57G||N||arc-staff, arc-vlbi||Data transfer node
|-
|arcbl19||64G||Intel Xeon E3-1275 v6||4/8||3800||10GbE||11T||57G||N||arc-staff, arc-vlbi, arc-f2f, arc-user||NFS server
|-
|arcbl20||256G||Intel Xeon E5-1650 v4||6/12||3600||10GbE||11T||65G||N||arc-staff, arc-vlbi||
|-
|arcbl21||64G||Intel Xeon E3-1275 v6||4/8||3800||10GbE||11T||57G||N||arc-staff, arc-vlbi||
|-
|arcbl22||256G||Intel Xeon E5-1650 v4||6/12||3600||10GbE||11T||65G||N||arc-staff, arc-vlbi, arc-f2f||
|-
|arcbl23||256G||Intel Xeon E5-1650 v4||6/12||3600||10GbE||11T||65G||N||arc-staff, arc-vlbi||VM
|-
|arcbl24||256G||Intel Xeon E5-1650 v4||6/12||3600||10GbE||11T||65G||N||arc-staff, arc-vlbi||
|-
|arcbl25||256G||Intel Xeon E5-1650 v4||6/12||3600||10GbE||11T||65G||N||arc-staff, arc-vlbi, arc-f2f||
|-
|arcbl26||256G||Intel Xeon E5-1650 v4||6/12||3600||10GbE||11T||65G||N||arc-staff, arc-vlbi, arc-f2f||
|-
|arcbl27||64G||Intel Xeon E3-1275 v6||4/8||3800||10GbE||15T||57G||N||arc-staff, arc-vlbi||
|-
|arcbl28||256G||Intel Xeon E5-1650 v4||6/12||3600||10GbE||15T||57G||N||arc-staff, arc-vlbi||
|-}

== Storage Nodes ==
{| class="wikitable"
|-
! Name !! RAM !! CPU !! Cores !! Clock !! Data Net !! RAID !! Space !! Storage !! export
|-
|arcnas2||32G||Intel Xeon Silver 4108||8/16||1800||10GbE||ARC-1883IX-24||91||12x10TB (HGST HUH721010ALE600) RAID6||/lustre/arcfs0/ost3
|-
|arcnas3||32G||Intel Xeon Silver 4108||8/16||1800||10GbE||ARC-1883IX-24||72,8||12x8TB (HGST HUH728080AL5200) RAID6 ||/lustre/arcfs0/ost0
|-
|arcnas4||16G||Intel XeonE5-2603v3||6/6||1600||10GbE||ARC-1284ML-24||36,4T||12x4TB (WDC WD4000F9YZ-09N20L1) RAID6||/lustre/arcfs0/ost1
|-
| || || || || || || ||91T||12x10TB (ST10000NM0086-2AA101) RAID6||/lustre/arcfs0/ost2
|-
|arcnas5||32G||Intel Xeon E5-2640 v4||10/20||2400||10GbE||Broadcom / LSI MegaRAID SAS-3 3108||255G||2x255GB RAID1||/lustre/arcfs0/mdt0
|}

The ARC cluster

2023-01-26T14:48:04Z

Kazi: /* Computing Nodes */

The ARC is equipped with a dedicated computer server connected with a high-speed optical fiber network to the outside world, allowing fast data transfer (10 Gbit/sec).

Presently we have 200 Tb of diskspace and one 26 nodes cluster (112 cores) dedicated to the ARC.

ALMA and CASA users can request access to the server and the disk space by sending an e-mail to ''arc-support at ira.inaf.it'' indicating the reason for the request.

[[File:Blade.jpg|thumbnail]]

== User policy==

New ARC users can access the Italian ARC node computing facilities by requesting a face-2-face visit (ALMA users only, through the ALMA Helpdesk) or by visiting the ARC node in Bologna (for any data-reduction-related issue to be solved in collaboration with the ARC staff). In both the cases they are requested to send an e-mail to help-desk@alma.inaf.it indicating the reason for the request.

Please notice that the request for a new account for a new requesting user implies that he/she (and/or his/her collaborators) visits the ARC for an induction on the ARC facilities usage and on issues related to data reduction with CASA both for ALMA or any other telescope. If the request is positively evaluated the visit details will be arranged via e-mail.

The account will guarantee the usage of the facilities and the support for 6 months.

Once the account expires the access to the data will be suspended and, after 1 month of quarantine ALL DATA WILL BE REMOVED. Only one gentle reminder will be send on account expiration.
Extensions of the account duration period could be considered on request (via e-mail). No visit is needed in case of account renewal.

The ARC members support is guaranteed for any ALMA-related issue.
For data-reduction-related issues that do not involve ALMA, the support (other than the technical support in the usage of the ARC computing facilities) is limited to the knowledge/experience and availability of the ARC members.

The same rules apply also to IRA staff members. IRA collaborators with temporary positions (i.e. students) can have an account for the entire duration of their position.

To ensure a well-balanced load on the cluster nodes please follow instructions about accessing the computer cluster

Queries can be issued via e-mail to help-desk@alma.inaf.it

Users will be automatically added to the arc-cluster-users@ira.inaf.it mailing list that will be used for any communication from our side.

== Accessing the computer cluster ==

Once you have obtained an '''ARC''' account at '''IRA''', you can access the computer cluster nodes from everywhere through host '''scheduler.ira.inaf.it.'''.
Using graphical applications on the cluster is possible through remote X access.
The accessible working nodes are listed in the table below.
You can enter a node for interactive work by typing:

<source lang="bash">ssh -X ''<node>''.ira.inaf.it</source>

''Useful tip: by typing 'hostname' you can know on which node you are''

[http://ganglia.ira.inaf.it/?r=hour&cs=&ce=&c=unspecified&h=&tab=m&vn=&hide-hf=false&m=load_one&sh=1&z=small&hc=4&host_regex=%5Earc&max_graphs=0&s=by+name Here] you can find some statistics about resources consumption on the arcblXX nodes.

== Using ARC storage ==

You need to change directory to access your ARC storage on the cluster:

<source lang="bash"> cd /iranet/homesarc/''username'' </source>

On each node you can also use local disks on path /local/work/username (if allocated) and /local/scratch

/local/scratch will be emptied on every reboot

Beware that local disks have '''no redundancy at all''', never leave important data on them

=== Mounting ARC storage on you workstation ===

On IRA workstations ARC home filesystem can be accessed on ''/iranet/homesarc''

On your laptop ARC filesystems can be seamlessly accessed with fuse-sshfs:

as root, install the package sshfs

<source lang="bash">
# on RedHat/Centos/ScientificLinux
yum install fuse-sshfs

# on Debian/Ubuntu
apt-get install sshfs
</source>

then, as user

<source lang="bash">sshfs storage.alma.inaf.it:/iranet/homesarc/yourhome /your/local/mount/point/</source>

By omitting /remote/path you can mount you home directory.

Be aware that this method is suboptimal for heavy input/output loads. Running disk-intensive applications directly on the arc cluster will result in a file access speed 10-50 times faster.

== Software packages available ==

Software available on ARC cluster could be listed typing the command ''setup-help'' or on [https://www.ira.inaf.it/wiki/index.php/Arcsoft this page]

== Computing Nodes ==
{| class="wikitable"
|-
! Name !! RAM !! CPU !! Cores !! Clock !! Data Net !! Work Disk !! Scratch Disk !! scheduler !! groups !! notes
|-
|arcbl01||256G||Intel Xeon E5-1650 v4||6/12||3600||10GbE||15T||57G||N||arc-staff, arc-vlbi, arc-f2f||
|
|arcbl17||64G||AMD Ryzen 7 1800X||8/16||3600||1GbE||3,5TB|| ||N||arc-staff, arc-vlbi||
|-
|arcbl18||64G||Intel Xeon E3-1275 v6||4/8||3800||10GbE||22T||57G||N||arc-staff, arc-vlbi||Data transfer node
|-
|arcbl19||64G||Intel Xeon E3-1275 v6||4/8||3800||10GbE||11T||57G||N||arc-staff, arc-vlbi, arc-f2f, arc-user||NFS server
|-
|arcbl20||256G||Intel Xeon E5-1650 v4||6/12||3600||10GbE||11T||65G||N||arc-staff, arc-vlbi||
|-
|arcbl21||64G||Intel Xeon E3-1275 v6||4/8||3800||10GbE||11T||57G||N||arc-staff, arc-vlbi||
|-
|arcbl22||256G||Intel Xeon E5-1650 v4||6/12||3600||10GbE||11T||65G||N||arc-staff, arc-vlbi, arc-f2f||
|-
|arcbl23||256G||Intel Xeon E5-1650 v4||6/12||3600||10GbE||11T||65G||N||arc-staff, arc-vlbi||VM
|-
|arcbl24||256G||Intel Xeon E5-1650 v4||6/12||3600||10GbE||11T||65G||N||arc-staff, arc-vlbi||
|-
|arcbl25||256G||Intel Xeon E5-1650 v4||6/12||3600||10GbE||11T||65G||N||arc-staff, arc-vlbi, arc-f2f||
|-
|arcbl26||256G||Intel Xeon E5-1650 v4||6/12||3600||10GbE||11T||65G||N||arc-staff, arc-vlbi, arc-f2f||
|-
|arcbl27||64G||Intel Xeon E3-1275 v6||4/8||3800||10GbE||15T||57G||N||arc-staff, arc-vlbi||
|-
|arcbl28||256G||Intel Xeon E5-1650 v4||6/12||3600||10GbE||15T||57G||N||arc-staff, arc-vlbi||
|-}

== Storage Nodes ==
{| class="wikitable"
|-
! Name !! RAM !! CPU !! Cores !! Clock !! Data Net !! RAID !! Space !! Storage !! export
|-
|arcnas2||32G||Intel Xeon Silver 4108||8/16||1800||10GbE||ARC-1883IX-24||91||12x10TB (HGST HUH721010ALE600) RAID6||/lustre/arcfs0/ost3
|-
|arcnas3||32G||Intel Xeon Silver 4108||8/16||1800||10GbE||ARC-1883IX-24||72,8||12x8TB (HGST HUH728080AL5200) RAID6 ||/lustre/arcfs0/ost0
|-
|arcnas4||16G||Intel XeonE5-2603v3||6/6||1600||10GbE||ARC-1284ML-24||36,4T||12x4TB (WDC WD4000F9YZ-09N20L1) RAID6||/lustre/arcfs0/ost1
|-
| || || || || || || ||91T||12x10TB (ST10000NM0086-2AA101) RAID6||/lustre/arcfs0/ost2
|-
|arcnas5||32G||Intel Xeon E5-2640 v4||10/20||2400||10GbE||Broadcom / LSI MegaRAID SAS-3 3108||255G||2x255GB RAID1||/lustre/arcfs0/mdt0
|}

The ARC cluster

2023-01-19T09:07:59Z

Kazi: /* Computing Nodes */

The ARC is equipped with a dedicated computer server connected with a high-speed optical fiber network to the outside world, allowing fast data transfer (10 Gbit/sec).

Presently we have 200 Tb of diskspace and one 26 nodes cluster (112 cores) dedicated to the ARC.

ALMA and CASA users can request access to the server and the disk space by sending an e-mail to ''arc-support at ira.inaf.it'' indicating the reason for the request.

[[File:Blade.jpg|thumbnail]]

== User policy==

New ARC users can access the Italian ARC node computing facilities by requesting a face-2-face visit (ALMA users only, through the ALMA Helpdesk) or by visiting the ARC node in Bologna (for any data-reduction-related issue to be solved in collaboration with the ARC staff). In both the cases they are requested to send an e-mail to help-desk@alma.inaf.it indicating the reason for the request.

Please notice that the request for a new account for a new requesting user implies that he/she (and/or his/her collaborators) visits the ARC for an induction on the ARC facilities usage and on issues related to data reduction with CASA both for ALMA or any other telescope. If the request is positively evaluated the visit details will be arranged via e-mail.

The account will guarantee the usage of the facilities and the support for 6 months.

Once the account expires the access to the data will be suspended and, after 1 month of quarantine ALL DATA WILL BE REMOVED. Only one gentle reminder will be send on account expiration.
Extensions of the account duration period could be considered on request (via e-mail). No visit is needed in case of account renewal.

The ARC members support is guaranteed for any ALMA-related issue.
For data-reduction-related issues that do not involve ALMA, the support (other than the technical support in the usage of the ARC computing facilities) is limited to the knowledge/experience and availability of the ARC members.

The same rules apply also to IRA staff members. IRA collaborators with temporary positions (i.e. students) can have an account for the entire duration of their position.

To ensure a well-balanced load on the cluster nodes please follow instructions about accessing the computer cluster

Queries can be issued via e-mail to help-desk@alma.inaf.it

Users will be automatically added to the arc-cluster-users@ira.inaf.it mailing list that will be used for any communication from our side.

== Accessing the computer cluster ==

Once you have obtained an '''ARC''' account at '''IRA''', you can access the computer cluster nodes from everywhere through host '''scheduler.ira.inaf.it.'''.
Using graphical applications on the cluster is possible through remote X access.
The accessible working nodes are listed in the table below.
You can enter a node for interactive work by typing:

<source lang="bash">ssh -X ''<node>''.ira.inaf.it</source>

''Useful tip: by typing 'hostname' you can know on which node you are''

[http://ganglia.ira.inaf.it/?r=hour&cs=&ce=&c=unspecified&h=&tab=m&vn=&hide-hf=false&m=load_one&sh=1&z=small&hc=4&host_regex=%5Earc&max_graphs=0&s=by+name Here] you can find some statistics about resources consumption on the arcblXX nodes.

== Using ARC storage ==

You need to change directory to access your ARC storage on the cluster:

<source lang="bash"> cd /iranet/homesarc/''username'' </source>

On each node you can also use local disks on path /local/work/username (if allocated) and /local/scratch

/local/scratch will be emptied on every reboot

Beware that local disks have '''no redundancy at all''', never leave important data on them

=== Mounting ARC storage on you workstation ===

On IRA workstations ARC home filesystem can be accessed on ''/iranet/homesarc''

On your laptop ARC filesystems can be seamlessly accessed with fuse-sshfs:

as root, install the package sshfs

<source lang="bash">
# on RedHat/Centos/ScientificLinux
yum install fuse-sshfs

# on Debian/Ubuntu
apt-get install sshfs
</source>

then, as user

<source lang="bash">sshfs storage.alma.inaf.it:/iranet/homesarc/yourhome /your/local/mount/point/</source>

By omitting /remote/path you can mount you home directory.

Be aware that this method is suboptimal for heavy input/output loads. Running disk-intensive applications directly on the arc cluster will result in a file access speed 10-50 times faster.

== Software packages available ==

Software available on ARC cluster could be listed typing the command ''setup-help'' or on [https://www.ira.inaf.it/wiki/index.php/Arcsoft this page]

== Computing Nodes ==
{| class="wikitable"
|-
! Name !! RAM !! CPU !! Cores !! Clock !! Data Net !! Work Disk !! Scratch Disk !! scheduler !! groups !! notes
|-
|arcbl17||64G||AMD Ryzen 7 1800X||8/16||3600||1GbE||3,5TB|| ||N||arc-staff, arc-vlbi||
|-
|arcbl18||64G||Intel Xeon E3-1275 v6||4/8||3800||10GbE||22T||57G||N||arc-staff, arc-vlbi||Data transfer node
|-
|arcbl19||64G||Intel Xeon E3-1275 v6||4/8||3800||10GbE||11T||57G||N||arc-staff, arc-vlbi, arc-f2f, arc-user||NFS server
|-
|arcbl20||256G||Intel Xeon E5-1650 v4||6/12||3600||10GbE||11T||65G||N||arc-staff, arc-vlbi||
|-
|arcbl21||64G||Intel Xeon E3-1275 v6||4/8||3800||10GbE||11T||57G||N||arc-staff, arc-vlbi||
|-
|arcbl22||256G||Intel Xeon E5-1650 v4||6/12||3600||10GbE||11T||65G||N||arc-staff, arc-vlbi, arc-f2f||
|-
|arcbl23||256G||Intel Xeon E5-1650 v4||6/12||3600||10GbE||11T||65G||N||arc-staff, arc-vlbi||VM
|-
|arcbl24||256G||Intel Xeon E5-1650 v4||6/12||3600||10GbE||11T||65G||N||arc-staff, arc-vlbi||
|-
|arcbl25||256G||Intel Xeon E5-1650 v4||6/12||3600||10GbE||11T||65G||N||arc-staff, arc-vlbi, arc-f2f||
|-
|arcbl26||256G||Intel Xeon E5-1650 v4||6/12||3600||10GbE||11T||65G||N||arc-staff, arc-vlbi, arc-f2f||
|-
|arcbl27||64G||Intel Xeon E3-1275 v6||4/8||3800||10GbE||15T||57G||N||arc-staff, arc-vlbi||
|-
|arcbl28||256G||Intel Xeon E5-1650 v4||6/12||3600||10GbE||15T||57G||N||arc-staff, arc-vlbi||
|-
|arcbl29||256G||Intel Xeon E5-1650 v4||6/12||3600||10GbE||15T||57G||N||arc-staff, arc-vlbi, arc-f2f||
|}

== Storage Nodes ==
{| class="wikitable"
|-
! Name !! RAM !! CPU !! Cores !! Clock !! Data Net !! RAID !! Space !! Storage !! export
|-
|arcnas2||32G||Intel Xeon Silver 4108||8/16||1800||10GbE||ARC-1883IX-24||91||12x10TB (HGST HUH721010ALE600) RAID6||/lustre/arcfs0/ost3
|-
|arcnas3||32G||Intel Xeon Silver 4108||8/16||1800||10GbE||ARC-1883IX-24||72,8||12x8TB (HGST HUH728080AL5200) RAID6 ||/lustre/arcfs0/ost0
|-
|arcnas4||16G||Intel XeonE5-2603v3||6/6||1600||10GbE||ARC-1284ML-24||36,4T||12x4TB (WDC WD4000F9YZ-09N20L1) RAID6||/lustre/arcfs0/ost1
|-
| || || || || || || ||91T||12x10TB (ST10000NM0086-2AA101) RAID6||/lustre/arcfs0/ost2
|-
|arcnas5||32G||Intel Xeon E5-2640 v4||10/20||2400||10GbE||Broadcom / LSI MegaRAID SAS-3 3108||255G||2x255GB RAID1||/lustre/arcfs0/mdt0
|}

The ARC cluster

2022-02-24T14:44:52Z

Kazi: /* Computing Nodes */

The ARC cluster

2019-12-04T16:21:17Z

Kazi: /* Nodes */

The ARC is equipped with a dedicated computer server connected with a high-speed optical fiber network to the outside world, allowing fast data transfer (10 Gbit/sec).

Presently we have 110 Tb of diskspace and one 15 nodes cluster (112 cores) dedicated to the ARC.

ALMA and CASA users can request access to the server and the disk space by sending an e-mail to ''arc-support at ira.inaf.it'' indicating the reason for the request.

[[File:Blade.jpg|thumbnail]]

== User policy==

New ARC users can access the Italian ARC node computing facilities by requesting a face-2-face visit (ALMA users only, through the ALMA Helpdesk) or by visiting the ARC node in Bologna (for any data-reduction-related issue to be solved in collaboration with the ARC staff). In both the cases they are requested to send an e-mail to help-desk@alma.inaf.it indicating the reason for the request.

Please notice that the request for a new account for a new requesting user implies that he/she (and/or his/her collaborators) visits the ARC for an induction on the ARC facilities usage and on issues related to data reduction with CASA both for ALMA or any other telescope. If the request is positively evaluated the visit details will be arranged via e-mail.

The account will guarantee the usage of the facilities and the support for 6 months.

Once the account expires the access to the data will be suspended and, after 1 month of quarantine ALL DATA WILL BE REMOVED. Only one gentle reminder will be send on account expiration.
Extensions of the account duration period could be considered on request (via e-mail). No visit is needed in case of account renewal.

The ARC members support is guaranteed for any ALMA-related issue.
For data-reduction-related issues that do not involve ALMA, the support (other than the technical support in the usage of the ARC computing facilities) is limited to the knowledge/experience and availability of the ARC members.

The same rules apply also to IRA staff members. IRA collaborators with temporary positions (i.e. students) can have an account for the entire duration of their position.

To ensure a well-balanced load on the cluster nodes please follow instructions about accessing the computer cluster

Queries can be issued via e-mail to help-desk@alma.inaf.it

Users will be automatically added to the arc-cluster-users@ira.inaf.it mailing list that will be used for any communication from our side.

== Accessing the computer cluster ==

Once you have obtained an '''ARC''' account at '''IRA''', you can access the computer cluster nodes from everywhere through host '''scheduler.ira.inaf.it.'''.
Using graphical applications on the cluster is possible through remote X access.
The accessible working nodes are listed in the table below. Never submit workloads to arcserv (control node) and arcnas1 (storage) as this can slow down the entire cluster.
You can enter a node for interactive work by typing:

<source lang="bash">ssh -tX scheduler.ira.inaf.it</source>

''Useful tip: by typing 'hostname' you can know on which node you are''

Access is done via a Slurm scheduler that redirects your job on the less-loaded node.

'''Jobs on the cluster are limited to a duration of 168 hours'''.

[http://ganglia.ira.inaf.it/?r=hour&cs=&ce=&c=unspecified&h=&tab=m&vn=&hide-hf=false&m=load_one&sh=1&z=small&hc=4&host_regex=%5Earc&max_graphs=0&s=by+name Here] you can find some statistics about resources consumption on the arcblXX nodes.

== Executing programs ==

You can execute programs in two ways:

in interactive mode - your command is immediately executed on the less-loaded node and standard input, output and error are linked to your terminal.

or scheduling a scheduler job - submit a job file ([https://slurm.schedmd.com/pdfs/summary.pdf here is a command summary])

== Using ARC storage ==

You need to change directory to access your ARC storage on the cluster:

<source lang="bash"> cd /iranet/homesarc/username </source>

On each node you can also use local disks on path /local/work/username (if allocated) and /local/scratch

/local/scratch will be emptied on every reboot

Beware that local disks have '''no redundancy at all''', never leave important data on them

=== Copying files to/from the ARC storage ===

==== via SCP ====

<source lang="bash">
# while running on a computer computer outside IRA

# trasferring from storage to your computer
scp user@alma-wan.ira.inaf.it:/remote/path /local/path

# from your computer to storage
scp /local/path user@alma-wan.ira.inaf.it:/remote/path

# while running on a computer computer inside IRA

# trasferring from storage to your computer
scp user@arcbl02.ira.inaf.it:/remote/path /local/path

# from your computer to storage
scp /local/path user@arcbl02.ira.inaf.it:/remote/path
</source>

==== via FTP ====

wget --ask-password ftp://your_username@alma-wan.ira.inaf.it//iranet/homesarc/your_username/file.fits

==== via HTTP ====

you can also download from your homesarc:

for example a file in /iranet/homesarc/your_username/public_html/file.dat

will be downloadable from http://alma-wan.ira.inaf.it/~your_username/file.dat

or you can make a symbolic link:

<source lang="bash">
cd /iranet/homesarc/your_username/public_html/
ln -s ../otherfile.dat
</source>

=== Mounting ARC storage on you workstation ===

On IRA workstations ARC home filesystem can be accessed on ''/iranet/homesarc''

On your laptop ARC filesystems can be seamlessly accessed with fuse-sshfs:

as root, install the package sshfs

<source lang="bash">
# on RedHat/Centos/ScientificLinux
yum install fuse-sshfs

# on Debian/Ubuntu
apt-get install sshfs
</source>

then, as user

<source lang="bash">sshfs storage.alma.inaf.it:/iranet/homesarc/yourhome /your/local/mount/point/</source>

By omitting /remote/path you can mount you home directory.

Be aware that this method is suboptimal for heavy input/output loads. Running disk-intensive applications directly on the arc cluster will result in a file access speed 10-50 times faster.

== Software packages available ==

Software available on ARC cluster could be listed typing the command ''setup-help''

{| class="wikitable"
|-
! Software package !! setup command !! launch command !! notes
|-
| CASA ||casapy-setup|| casapy || data reduction package http://casa.nrao.edu/
|-
| Miriad ||miriad-setup|| miriad || data reduction package http://www.atnf.csiro.au/computing/software/miriad/
|-
|aips||aips-setup|| || http://www.aips.nrao.edu/index.shtml
|-
|analysis utils||analysisUtils-setup|| ||
|-
|analytic infall||analytic_infall-setup||
|-
|astron||astron-setup|| ||
|-
|Coyote library||coyote-setup|| ||
|-
|fits Viewer||fv-setup|| ||
|-
|GCC Compiler||gcc-setup||
|-
|Gildas||gildas-setup|| ||http://www.iram.fr/IRAMFR/GILDAS/
|-
|Healpix||healpix-setup|| ||http://healpix.jpl.nasa.gov/
|-
|IDL||idl-setup|| ||http://www.exelisvis.com/ProductsServices/IDL.aspx
|-
|heasoft||heasoft-setup|| ||http://heasarc.nasa.gov/lheasoft/
|-
|QA2||qa2-setup|| ||
|-
|Ratran||ratran-setup|| ||http://www.sron.rug.nl/~vdtak/ratran/frames.html
|-
|Starlink||starlink-setup|| ||http://starlink.jach.hawaii.edu/starlink
|}

== Nodes ==
{| class="wikitable"
|-
! Name !! RAM !! CPU !! Cores !! Clock !! Data Net !! Work Disk !! Scratch Disk !! scheduler !! groups !! notes
|-
|arcbl01||32G||Intel Xeon E5-2637 v3||2 x 4/8||3500||10GbE||1TB||1TB||N||*||
|-
|arcbl02||8G||AMD Opteron 2352||8||2100||10GbE||34G|| ||Y||*||reserved for file transfer
|-
|arcbl03||8G||AMD Opteron 2352||8||2100||10GbE||34G|| ||Y||*||reserved for nfs export
|-
|arcbl04||8G||AMD Opteron 2352||8||2100||10GbE||34G|| ||Y||*||
|-
|arcbl05||8G||AMD Opteron 2352||8||2100||10GbE||1T|| ||Y||*||
|-
|arcbl06||8G||AMD Opteron 2352||8||2100||10GbE||34G|| ||Y||*||
|-
|arcbl07||8G||AMD Opteron 2352||8||2100||10GbE||34G|| ||Y||*||
|-
|arcbl08||8G||AMD Opteron 2352||8||2100||10GbE||34G|| ||Y||*||disabled
|-
|arcbl09||8G||AMD Opteron 2352||8||2100||10GbE||34G|| ||Y||*||disabled
|-
|arcbl10||32G||Intel Xeon E5-2637 v3||2 x 4/8||3500||10GbE||1T||1T||N||arc-staff, arc-vlbi||
|-
|arcbl11||8G||AMD Opteron 2352||8||2100||10GbE||34G|| ||N||arc-staff, arc-vlbi||
|-
|arcbl12||16G||AMD Opteron 2352||8||2100||10GbE||34G|| ||N||arc-staff, arc-vlbi, arc-f2f||
|-
|arcbl13||16G||AMD Opteron 2387||4||2800||10GbE||136G|| ||N||arc-staff, arc-vlbi, arc-f2f||
|-
|arcbl17||64G||AMD Ryzen 7 1800X||8/16||3600||1GbE||3,5TB|| ||N||arc-staff, arc-vlbi||
|-
|arcbl18||64G||Intel Xeon E3-1275 v6||4/8||3800||10GbE||22T||57G||N||arc-staff, arc-vlbi||
|-
|arcbl19||64G||Intel Xeon E3-1275 v6||4/8||3800||10GbE||11T||57G||N||arc-staff, arc-vlbi, arc-f2f||
|-
|arcbl20||256G||Intel Xeon E5-1650 v4||6/12||3600||10GbE||11T||65G||N||arc-staff, arc-vlbi, arc-f2f||
|-
|arcbl21||64G||Intel Xeon E3-1275 v6||4/8||3800||10GbE||11T||57G||N||arc-staff, arc-vlbi, arc-f2f||
|-
|arcbl22||256G||Intel Xeon E5-1650 v4||6/12||3600||10GbE||11T||65G||N||arc-staff, arc-vlbi||
|-
|arcbl23||256G||Intel Xeon E5-1650 v4||6/12||3600||10GbE||11T||65G||N||arc-staff, arc-vlbi||
|-
|arcbl24||256G||Intel Xeon E5-1650 v4||6/12||3600||10GbE||11T||65G||N||arc-staff, arc-vlbi||
|-
|arcbl25||256G||Intel Xeon E5-1650 v4||6/12||3600||10GbE||11T||65G||N||arc-staff, arc-vlbi||
|-
|arcbl26||256G||Intel Xeon E5-1650 v4||6/12||3600||10GbE||11T||65G||N||arc-staff, arc-vlbi||
|-
|arcbl27||256G||Intel Xeon E3-1275 v6||4/8||3800||10GbE||15T||57G||N||arc-staff, arc-vlbi||
|-
|arcbl28||256G||Intel Xeon E3-1275 v6||4/8||3800||10GbE||15T||57G||N||arc-staff, arc-vlbi||
|}

The ARC cluster

2019-10-28T09:54:57Z

Kazi:

The ARC is equipped with a dedicated computer server connected with a high-speed optical fiber network to the outside world, allowing fast data transfer (10 Gbit/sec).

Presently we have 110 Tb of diskspace and one 15 nodes cluster (112 cores) dedicated to the ARC.

ALMA and CASA users can request access to the server and the disk space by sending an e-mail to ''arc-support at ira.inaf.it'' indicating the reason for the request.

[[File:Blade.jpg|thumbnail]]

== User policy==

New ARC users can access the Italian ARC node computing facilities by requesting a face-2-face visit (ALMA users only, through the ALMA Helpdesk) or by visiting the ARC node in Bologna (for any data-reduction-related issue to be solved in collaboration with the ARC staff). In both the cases they are requested to send an e-mail to help-desk@alma.inaf.it indicating the reason for the request.

Please notice that the request for a new account for a new requesting user implies that he/she (and/or his/her collaborators) visits the ARC for an induction on the ARC facilities usage and on issues related to data reduction with CASA both for ALMA or any other telescope. If the request is positively evaluated the visit details will be arranged via e-mail.

The account will guarantee the usage of the facilities and the support for 6 months.

Once the account expires the access to the data will be suspended and, after 1 month of quarantine ALL DATA WILL BE REMOVED. Only one gentle reminder will be send on account expiration.
Extensions of the account duration period could be considered on request (via e-mail). No visit is needed in case of account renewal.

The ARC members support is guaranteed for any ALMA-related issue.
For data-reduction-related issues that do not involve ALMA, the support (other than the technical support in the usage of the ARC computing facilities) is limited to the knowledge/experience and availability of the ARC members.

The same rules apply also to IRA staff members. IRA collaborators with temporary positions (i.e. students) can have an account for the entire duration of their position.

To ensure a well-balanced load on the cluster nodes please follow instructions about accessing the computer cluster

Queries can be issued via e-mail to help-desk@alma.inaf.it

Users will be automatically added to the arc-cluster-users@ira.inaf.it mailing list that will be used for any communication from our side.

== Accessing the computer cluster ==

Once you have obtained an '''ARC''' account at '''IRA''', you can access the computer cluster nodes from everywhere through host '''scheduler.ira.inaf.it.'''.
Using graphical applications on the cluster is possible through remote X access.
The accessible working nodes are listed in the table below. Never submit workloads to arcserv (control node) and arcnas1 (storage) as this can slow down the entire cluster.
You can enter a node for interactive work by typing:

<source lang="bash">ssh -tX scheduler.ira.inaf.it</source>

''Useful tip: by typing 'hostname' you can know on which node you are''

Access is done via a Slurm scheduler that redirects your job on the less-loaded node.

'''Jobs on the cluster are limited to a duration of 168 hours'''.

[http://ganglia.ira.inaf.it/?r=hour&cs=&ce=&c=unspecified&h=&tab=m&vn=&hide-hf=false&m=load_one&sh=1&z=small&hc=4&host_regex=%5Earc&max_graphs=0&s=by+name Here] you can find some statistics about resources consumption on the arcblXX nodes.

== Executing programs ==

You can execute programs in two ways:

in interactive mode - your command is immediately executed on the less-loaded node and standard input, output and error are linked to your terminal.

or scheduling a scheduler job - submit a job file ([https://slurm.schedmd.com/pdfs/summary.pdf here is a command summary])

== Using ARC storage ==

You need to change directory to access your ARC storage on the cluster:

<source lang="bash"> cd /iranet/homesarc/username </source>

On each node you can also use local disks on path /local/work/username (if allocated) and /local/scratch

/local/scratch will be emptied on every reboot

Beware that local disks have '''no redundancy at all''', never leave important data on them

=== Copying files to/from the ARC storage ===

==== via SCP ====

<source lang="bash">
# while running on a computer computer outside IRA

# trasferring from storage to your computer
scp user@alma-wan.ira.inaf.it:/remote/path /local/path

# from your computer to storage
scp /local/path user@alma-wan.ira.inaf.it:/remote/path

# while running on a computer computer inside IRA

# trasferring from storage to your computer
scp user@arcbl02.ira.inaf.it:/remote/path /local/path

# from your computer to storage
scp /local/path user@arcbl02.ira.inaf.it:/remote/path
</source>

==== via FTP ====

wget --ask-password ftp://your_username@alma-wan.ira.inaf.it//iranet/homesarc/your_username/file.fits

==== via HTTP ====

you can also download from your homesarc:

for example a file in /iranet/homesarc/your_username/public_html/file.dat

will be downloadable from http://alma-wan.ira.inaf.it/~your_username/file.dat

or you can make a symbolic link:

<source lang="bash">
cd /iranet/homesarc/your_username/public_html/
ln -s ../otherfile.dat
</source>

=== Mounting ARC storage on you workstation ===

On IRA workstations ARC home filesystem can be accessed on ''/iranet/homesarc''

On your laptop ARC filesystems can be seamlessly accessed with fuse-sshfs:

as root, install the package sshfs

<source lang="bash">
# on RedHat/Centos/ScientificLinux
yum install fuse-sshfs

# on Debian/Ubuntu
apt-get install sshfs
</source>

then, as user

<source lang="bash">sshfs storage.alma.inaf.it:/iranet/homesarc/yourhome /your/local/mount/point/</source>

By omitting /remote/path you can mount you home directory.

Be aware that this method is suboptimal for heavy input/output loads. Running disk-intensive applications directly on the arc cluster will result in a file access speed 10-50 times faster.

== Software packages available ==

Software available on ARC cluster could be listed typing the command ''setup-help''

{| class="wikitable"
|-
! Software package !! setup command !! launch command !! notes
|-
| CASA ||casapy-setup|| casapy || data reduction package http://casa.nrao.edu/
|-
| Miriad ||miriad-setup|| miriad || data reduction package http://www.atnf.csiro.au/computing/software/miriad/
|-
|aips||aips-setup|| || http://www.aips.nrao.edu/index.shtml
|-
|analysis utils||analysisUtils-setup|| ||
|-
|analytic infall||analytic_infall-setup||
|-
|astron||astron-setup|| ||
|-
|Coyote library||coyote-setup|| ||
|-
|fits Viewer||fv-setup|| ||
|-
|GCC Compiler||gcc-setup||
|-
|Gildas||gildas-setup|| ||http://www.iram.fr/IRAMFR/GILDAS/
|-
|Healpix||healpix-setup|| ||http://healpix.jpl.nasa.gov/
|-
|IDL||idl-setup|| ||http://www.exelisvis.com/ProductsServices/IDL.aspx
|-
|heasoft||heasoft-setup|| ||http://heasarc.nasa.gov/lheasoft/
|-
|QA2||qa2-setup|| ||
|-
|Ratran||ratran-setup|| ||http://www.sron.rug.nl/~vdtak/ratran/frames.html
|-
|Starlink||starlink-setup|| ||http://starlink.jach.hawaii.edu/starlink
|}

== Nodes ==
{| class="wikitable"
|-
! Name !! RAM !! CPU !! Cores !! Clock !! Data Net !! Work Disk !! Scratch Disk !! scheduler !! groups !! notes
|-
|arcbl01||32G||Intel Xeon E5-2637 v3||2 x 4/8||3500||10GbE||1TB||1TB||N||*||
|-
|arcbl02||8G||AMD Opteron 2352||8||2100||10GbE||34G|| ||Y||*||reserved for file transfer
|-
|arcbl03||8G||AMD Opteron 2352||8||2100||10GbE||34G|| ||Y||*||reserved for nfs export
|-
|arcbl04||8G||AMD Opteron 2352||8||2100||10GbE||34G|| ||Y||*||
|-
|arcbl05||8G||AMD Opteron 2352||8||2100||10GbE||1T|| ||Y||*||
|-
|arcbl06||8G||AMD Opteron 2352||8||2100||10GbE||34G|| ||Y||*||
|-
|arcbl07||8G||AMD Opteron 2352||8||2100||10GbE||34G|| ||Y||*||
|-
|arcbl08||8G||AMD Opteron 2352||8||2100||10GbE||34G|| ||Y||*||disabled
|-
|arcbl09||8G||AMD Opteron 2352||8||2100||10GbE||34G|| ||Y||*||disabled
|-
|arcbl10||32G||Intel Xeon E5-2637 v3||2 x 4/8||3500||10GbE||1T||1T||N||arc-staff, arc-vlbi||
|-
|arcbl11||8G||AMD Opteron 2352||8||2100||10GbE||34G|| ||N||arc-staff, arc-vlbi||
|-
|arcbl12||16G||AMD Opteron 2352||8||2100||10GbE||34G|| ||N||arc-staff, arc-vlbi, arc-f2f||
|-
|arcbl13||16G||AMD Opteron 2387||4||2800||10GbE||136G|| ||N||arc-staff, arc-vlbi, arc-f2f||
|-
|arcbl17||64G||AMD Ryzen 7 1800X||8/16||3600||1GbE||3,5TB|| ||N||arc-staff, arc-vlbi||
|-
|arcbl18||64G||Intel Xeon E3-1275 v6||4/8||3800||10GbE||22T||57G||N||arc-staff, arc-vlbi||
|-
|arcbl19||64G||Intel Xeon E3-1275 v6||4/8||3800||10GbE||11T||57G||N||arc-staff, arc-vlbi, arc-f2f||
|-
|arcbl20||256G||Intel Xeon E5-1650 v4||6/12||3600||10GbE||11T||65G||N||arc-staff, arc-vlbi||
|-
|arcbl21||64G||Intel Xeon E3-1275 v6||4/8||3800||10GbE||11T||57G||N||arc-staff, arc-vlbi, arc-f2f||
|-
|arcbl22||256G||Intel Xeon E5-1650 v4||6/12||3600||10GbE||11T||65G||N||arc-staff, arc-vlbi||
|-
|arcbl23||256G||Intel Xeon E5-1650 v4||6/12||3600||10GbE||11T||65G||N||arc-staff, arc-vlbi||
|-
|arcbl24||256G||Intel Xeon E5-1650 v4||6/12||3600||10GbE||11T||65G||N||arc-staff, arc-vlbi||
|-
|arcbl25||256G||Intel Xeon E5-1650 v4||6/12||3600||10GbE||11T||65G||N||arc-staff, arc-vlbi||
|-
|arcbl26||256G||Intel Xeon E5-1650 v4||6/12||3600||10GbE||11T||65G||N||arc-staff, arc-vlbi||
|-
|arcbl27||256G||Intel Xeon E3-1275 v6||4/8||3800||10GbE||15T||57G||N||*||
|-
|arcbl28||256G||Intel Xeon E3-1275 v6||4/8||3800||10GbE||15T||57G||N||*||
|}

Theses

2017-11-23T10:08:08Z

Kazi:

== Available projects ==

* '''Titolo: Una nuova epoca degli studi dell'effetto Sunyaev Zel'dovich con ALMA'''

Gli ammassi di galassie si trovano nei nodi della rete cosmica e sono le
più grandi strutture in equilibrio dinamico nell'Universo. Le attività di
merger durante la formazione di queste strutture lasciano tracce nella
morfologia del gas diffuso intra-ammasso (ICM). Questo plasma, formando la
maggior parte della massa barionica di un'ammasso, può essere studiato
tramite osservazioni in banda X e sfruttando l'effetto Sunyaev-Zel'dovich
(SZ). L'effetto SZ è una distorsione dello spettro della radiazione
cosmica di fondo (CMB) causato dallo scattering Compton inverso dei fotoni
CMB all'interazione con gli elettroni caldi nell'ICM. Inoltre, l'effetto
SZ e' proporzionale alla pressione degli elettroni integrata e quindi ci
permette non solo una misura dell'energia termica degli ammassi ma anche
del loro stato morfologico.
Lo scopo di questa tesi è di studiare la struttura di un ammasso di
galassie attraverso l'effetto SZ usando dati di ALMA (RXCJ1347, Kitayama et
al. 2016) per modellare la sua morfologia. Nello specifico, sarà condotta
la riduzione dei dati, la costruzione di modelli di emissione dell'ammasso
e il confronto coi dati. Qualora i resultati su
RXCJ1347 e il tempo a disposizione lo consentano, sara' possibile
considerarne l'applicazione anche ai dati ALMA proprietari non ancora
pubblicati.
Questa tesi e' ottima per chi vuole imparare a trattare dati
interferometrici e richiede un investimento di tempo di minimo 6 mesi.

'''Contatti: Sandra Burkutean burkutean@ira.inaf.it, Marcella Massardi massardi@ira.inaf.it'''

'''Referente UniBO: Myriam Gitti'''

*'''Titolo: Giant molecular clouds properties along the bar of NGC3627'''
ALMA has the ability to resolve star-forming structures
in nearby galaxies with unprecedented sensitivity.
Detailed studies of Giant molecular clouds (GMC) previously possible only in
the Milky Way can be now done on GMC in nearby galaxies.
ALMA observations of two CO transitions (CO(1-0) and CO(2-1))
have been recently taken in the bar region of NGC3627
NGC3627 is a nearby, face-on, galaxy, with a prominent bar structure,
well observed at different frequencies.
The spatial resolution achieved at 230 GHz (CO(2-1)) is of ~30 pc.
It is possible to conduct a detailed study of the properties
of GMC in different environments: the nucleus of the galaxy,
the bar regions, the ends of the bar, the inner rings.

Lavoro:
Calibrazione e imaging dei dati ALMA.
Analisi dei dati e estrazione delle proprieta' delle GMCs.

Durata: > 6 mesi

'''Referente IRA-ARC: Rosita Paladino (paladino@ira.inaf.it)'''

'''Referente UniBO: Cristian Vignali'''

*'''Title: Unveiling the nature of high-redshift radio galaxies in the radio and millimeter band.'''

Scientific Rationale:
High-redshift radio galaxies (HzRGs) are among the most massive galaxies in the early
Universe. They have traditionally been identified by the ultra-steep spectrum of their easily detectable radio continuum, which served as a beacon for tracing
the faint host galaxy environment. HzRGs have been observed to be the signposts of large overdensities in the early Universe, the
so-called protoclusters that are believed to be the ancestors of local rich clusters. There are strong evidences that HzRGs in the center of high-z clusters are the
probable progenitor of the local Brightest Cluster Galaxies. HzRGs are therefore an ideal tool for probing the formation of
BCGs and the AGN activity in the host galaxies in premordial cluster environment.

Goals:
Clarifying the still unknown continuum millimeter and puzzling radio properties of a sample of HzRGs in the Southern Hemisphere: identification of source components (core, jets, lobes) and possibly the emission mechanisms (thermal or non-thermal?).
Studying the cold molecular gas content which is the raw ingredient for star formation and potential fuel for the AGN: how does it relate with the radio morphology?

Methods:
Analysis of archival ALMA millimeter observations, and VLA/ATCA radio data.

Acquired skills:
Archive mining, CASA imaging, analysis tools (python scripts, KAFE software)
Depending on the available time, ALMA data calibration processes

Required working time: > 6 months

'''IRA-ARC Referent: Elisabetta Liuzzo (liuzzo@ira.inaf.it)'''--
'''UniBO Referent: Myriam Gitti'''

*'''Title: The origin of the mini-starburst in the War-and-Peace Nebula'''

Aim:
To look for signs of cloud-cloud collisions in one of the
most active SF complexes in our Galaxy. This region, aka NGC6357,
contains 3 very massive open clusters, hosting some of the most
massive stars known to exist. The formation of these star clusters
may have been triggered by the collision of two or more molecular
clouds. The effects of this should be visible in the morphology and
kinematics of the molecular gas.

Available material:
maps of the entire complex in:
12CO(3-2) and 13CO(3-2) (JCMT);
Near-IR (JHK,H2) (UKIRT);
mid-IR (GLIMPSE);
dust-continuum emission (450mum, 850mum: SCUBA2; Herschel Hi-GAL)

Duration: 6 months

'''Supervisors:'''

'''IRA-ARC: Jan Brand (brand@ira.inaf.it), Andrea Giannetti (agianne@ira.inaf.it)'''

'''Arcetri: Fabrizio Massi (fmassi@arcetri.astro.it)'''

*'''Title: Dust polarization study of star-forming objects in the Orion filament'''

Magnetic fields are found to play an important role in filamentary shaped molecular clouds and most probably also in prestellar cores and young stellar objects. So far only very few polarimetric observations have been carried out at the high angular resolution and sensitivity necessary to capture single star-forming objects. The Laurea thesis will aim at retrieving the polarimetric properties of three young star-forming objects in the Orion filament using Archival ALMA data and relate this to the gravitational energy and outflow properties.

Lavoro:
Calibrazione e imaging di dati ALMA in polarizzazione.
Analisi dati polarizzazione, del dust continuum e dati CO (JCMT, Archive) per indagare la relazione del campo magnetico rispetto agli effetti di gravita' e outflow.

Durata: > 6 mesi da iniziare da Marzo 2018 in poi

'''Referente IRA-ARC: Kazi Rygl (kazi@ira.inaf.it) e Rosita Paladino (paladino@ira.inaf.it)'''

'''Referente UniBo: Francesca Pozzi (f.pozzi@unibo.it)'''

== On going theses ==

- '''Giovanni Sabatini ''': 'Establishing a timeline for the high-mass star formation process' PhD thesis, supervisor J. Brand, A. Giannetti, G. Giovannini

- '''Ilaria Ruffa ''': 'The AGN fueling/feedback cycle: a multi-phase study of a sample of local radio galaxies' PhD thesis, supervisors I. Prandoni, R. Laing, G. Giovannini

- '''Vincenzo Galluzzi''': 'Multi-frequency study of radio source polarimetry in millimetric bands' PhD thesis, supervisor M. Massardi, L. Gregorini

== Submitted theses ==

-''' Giovanni Sabatini ''', 'Unveiling the inner morphology and gas kinematics of NGC5135 with ALMA', 2017 Master Thesis, supervisor A. Ciamatti, C. Gruppioni, M. Massardi, F. Pozzi

- ''' Francesco Fragnito ''', 'Kinematics modelling of molecular gas in NGC 3100', 2017 Master Thesis, supervisor G. Giovannini, I. Prandoni, R. Paladino,

- ''' Matilde Mingozzi ''', 'Investigating the AGN-starburst connection in a nearby Seyfert galaxy with ALMA and multiwavelength data', 2016 Master Thesis, supervisor F. Pozzi, L. Vallini, A. Mignano.

- '''Ilaria Riuffa''': 'Multi wavelengths properties of a sample of obscured AGNs', 2016 Master Thesis,
Supervisor: C. Vignali, A. Mignano

- '''Eleonora Bianchi''': 'Observability of high density tracing molecular lines in lensed galaxies with ALMA' 2014 master thesis, supervisor M. Massardi, L. Gregorini

- '''Chiara Verdirame''': 'The core mass function in star-forming region NGC 6357', 2014 Master thesis, supervisor J. Brand, A. Giannetti [L. Gregorini]

- '''Andrea Giannetti''': 'The evolution of massive clumps in star forming regions', 2014 PhD thesis, supervisor J. Brand [L. Gregorini]

- '''Daria Dall'Olio''': 'IRAS16293-2422 as seen with ALMA: chemistry and morphology', 2013 Master thesis, supervisor J. Boissier [L. Gregorini], in collaboration with J. Brand, A. Mignano, R. Paladino

- '''Andrea Giannetti''': 'A detailed study of molecular clouds and star formation associated with the Galactic HII region G353.2+0.9', 2010 Master thesis, supervisor J. Brand [L. Gregorini]

Theses

2017-11-22T11:46:22Z

Kazi:

== Available projects ==

* '''Titolo: Una nuova epoca degli studi dell'effetto Sunyaev Zel'dovich con ALMA'''

Gli ammassi di galassie si trovano nei nodi della rete cosmica e sono le
più grandi strutture in equilibrio dinamico nell'Universo. Le attività di
merger durante la formazione di queste strutture lasciano tracce nella
morfologia del gas diffuso intra-ammasso (ICM). Questo plasma, formando la
maggior parte della massa barionica di un'ammasso, può essere studiato
tramite osservazioni in banda X e sfruttando l'effetto Sunyaev-Zel'dovich
(SZ). L'effetto SZ è una distorsione dello spettro della radiazione
cosmica di fondo (CMB) causato dallo scattering Compton inverso dei fotoni
CMB all'interazione con gli elettroni caldi nell'ICM. Inoltre, l'effetto
SZ e' proporzionale alla pressione degli elettroni integrata e quindi ci
permette non solo una misura dell'energia termica degli ammassi ma anche
del loro stato morfologico.
Lo scopo di questa tesi è di studiare la struttura di un ammasso di
galassie attraverso l'effetto SZ usando dati di ALMA (RXCJ1347, Kitayama et
al. 2016) per modellare la sua morfologia. Nello specifico, sarà condotta
la riduzione dei dati, la costruzione di modelli di emissione dell'ammasso
e il confronto coi dati. Qualora i resultati su
RXCJ1347 e il tempo a disposizione lo consentano, sara' possibile
considerarne l'applicazione anche ai dati ALMA proprietari non ancora
pubblicati.
Questa tesi e' ottima per chi vuole imparare a trattare dati
interferometrici e richiede un investimento di tempo di minimo 6 mesi.

'''Contatti: Sandra Burkutean burkutean@ira.inaf.it, Marcella Massardi massardi@ira.inaf.it'''

'''Referente UniBO: Myriam Gitti'''

*'''Titolo: Giant molecular clouds properties along the bar of NGC3627'''
ALMA has the ability to resolve star-forming structures
in nearby galaxies with unprecedented sensitivity.
Detailed studies of Giant molecular clouds (GMC) previously possible only in
the Milky Way can be now done on GMC in nearby galaxies.
ALMA observations of two CO transitions (CO(1-0) and CO(2-1))
have been recently taken in the bar region of NGC3627
NGC3627 is a nearby, face-on, galaxy, with a prominent bar structure,
well observed at different frequencies.
The spatial resolution achieved at 230 GHz (CO(2-1)) is of ~30 pc.
It is possible to conduct a detailed study of the properties
of GMC in different environments: the nucleus of the galaxy,
the bar regions, the ends of the bar, the inner rings.

Lavoro:
Calibrazione e imaging dei dati ALMA.
Analisi dei dati e estrazione delle proprieta' delle GMCs.

Durata: > 6 mesi

'''Referente IRA-ARC: Rosita Paladino (paladino@ira.inaf.it)'''

'''Referente UniBO: Cristian Vignali'''

*'''Title: Unveiling the nature of high-redshift radio galaxies in the radio and millimeter band.'''

Scientific Rationale:
High-redshift radio galaxies (HzRGs) are among the most massive galaxies in the early
Universe. They have traditionally been identified by the ultra-steep spectrum of their easily detectable radio continuum, which served as a beacon for tracing
the faint host galaxy environment. HzRGs have been observed to be the signposts of large overdensities in the early Universe, the
so-called protoclusters that are believed to be the ancestors of local rich clusters. There are strong evidences that HzRGs in the center of high-z clusters are the
probable progenitor of the local Brightest Cluster Galaxies. HzRGs are therefore an ideal tool for probing the formation of
BCGs and the AGN activity in the host galaxies in premordial cluster environment.

Goals:
Clarifying the still unknown continuum millimeter and puzzling radio properties of a sample of HzRGs in the Southern Hemisphere: identification of source components (core, jets, lobes) and possibly the emission mechanisms (thermal or non-thermal?).
Studying the cold molecular gas content which is the raw ingredient for star formation and potential fuel for the AGN: how does it relate with the radio morphology?

Methods:
Analysis of archival ALMA millimeter observations, and VLA/ATCA radio data.

Acquired skills:
Archive mining, CASA imaging, analysis tools (python scripts, KAFE software)
Depending on the available time, ALMA data calibration processes

Required working time: > 6 months

'''IRA-ARC Referent: Elisabetta Liuzzo (liuzzo@ira.inaf.it)'''--
'''UniBO Referent: Myriam Gitti'''

*'''Title: The origin of the mini-starburst in the War-and-Peace Nebula'''

Aim:
To look for signs of cloud-cloud collisions in one of the
most active SF complexes in our Galaxy. This region, aka NGC6357,
contains 3 very massive open clusters, hosting some of the most
massive stars known to exist. The formation of these star clusters
may have been triggered by the collision of two or more molecular
clouds. The effects of this should be visible in the morphology and
kinematics of the molecular gas.

Available material:
maps of the entire complex in:
12CO(3-2) and 13CO(3-2) (JCMT);
Near-IR (JHK,H2) (UKIRT);
mid-IR (GLIMPSE);
dust-continuum emission (450mum, 850mum: SCUBA2; Herschel Hi-GAL)

Duration: 6 months

'''Supervisors:'''

'''IRA-ARC: Jan Brand (brand@ira.inaf.it), Andrea Giannetti (agianne@ira.inaf.it)'''

'''Arcetri: Fabrizio Massi (fmassi@arcetri.astro.it)'''

*'''Title: Dust polarization study of star-forming objects in the Orion filament'''

Magnetic fields are found to play an important role in filamentary shaped molecular clouds and most probably also in prestellar cores and young stellar objects. So far only very few polarimetric observations have been carried out at the high angular resolution and sensitivity necessary to capture single star-forming objects. The Laurea thesis will aim at retrieving the polarimetric properties of three young star-forming objects in the Orion filament using Archival ALMA data and relate this to the gravitational energy and outflow properties.

Lavoro:
Calibrazione e imaging di dati ALMA in polarizzazione.
Analisi dati polarizzazione, del dust continuum e dati CO (JCMT, Archive) per indagare la relazione del campo magnetico rispetto agli effetti di gravita' e outflow.

Durata: > 6 mesi da iniziare da Marzo 2018 in poi

'''Referente IRA-ARC: Kazi Rygl (kazi@ira.inaf.it) e Rosita Paladino (paladino@ira.inaf.it)'''

'''Referente UniBo: TBD'''

== On going theses ==

- '''Giovanni Sabatini ''': 'Establishing a timeline for the high-mass star formation process' PhD thesis, supervisor J. Brand, A. Giannetti, G. Giovannini

- '''Ilaria Ruffa ''': 'The AGN fueling/feedback cycle: a multi-phase study of a sample of local radio galaxies' PhD thesis, supervisors I. Prandoni, R. Laing, G. Giovannini

- '''Vincenzo Galluzzi''': 'Multi-frequency study of radio source polarimetry in millimetric bands' PhD thesis, supervisor M. Massardi, L. Gregorini

== Submitted theses ==

-''' Giovanni Sabatini ''', 'Unveiling the inner morphology and gas kinematics of NGC5135 with ALMA', 2017 Master Thesis, supervisor A. Ciamatti, C. Gruppioni, M. Massardi, F. Pozzi

- ''' Francesco Fragnito ''', 'Kinematics modelling of molecular gas in NGC 3100', 2017 Master Thesis, supervisor G. Giovannini, I. Prandoni, R. Paladino,

- ''' Matilde Mingozzi ''', 'Investigating the AGN-starburst connection in a nearby Seyfert galaxy with ALMA and multiwavelength data', 2016 Master Thesis, supervisor F. Pozzi, L. Vallini, A. Mignano.

- '''Ilaria Riuffa''': 'Multi wavelengths properties of a sample of obscured AGNs', 2016 Master Thesis,
Supervisor: C. Vignali, A. Mignano

- '''Eleonora Bianchi''': 'Observability of high density tracing molecular lines in lensed galaxies with ALMA' 2014 master thesis, supervisor M. Massardi, L. Gregorini

- '''Chiara Verdirame''': 'The core mass function in star-forming region NGC 6357', 2014 Master thesis, supervisor J. Brand, A. Giannetti [L. Gregorini]

- '''Andrea Giannetti''': 'The evolution of massive clumps in star forming regions', 2014 PhD thesis, supervisor J. Brand [L. Gregorini]

- '''Daria Dall'Olio''': 'IRAS16293-2422 as seen with ALMA: chemistry and morphology', 2013 Master thesis, supervisor J. Boissier [L. Gregorini], in collaboration with J. Brand, A. Mignano, R. Paladino

- '''Andrea Giannetti''': 'A detailed study of molecular clouds and star formation associated with the Galactic HII region G353.2+0.9', 2010 Master thesis, supervisor J. Brand [L. Gregorini]

Theses

2017-11-21T20:09:20Z

Kazi:

== Available projects ==

* '''Titolo: Una nuova epoca degli studi dell'effetto Sunyaev Zel'dovich con ALMA'''

Gli ammassi di galassie si trovano nei nodi della rete cosmica e sono le
più grandi strutture in equilibrio dinamico nell'Universo. Le attività di
merger durante la formazione di queste strutture lasciano tracce nella
morfologia del gas diffuso intra-ammasso (ICM). Questo plasma, formando la
maggior parte della massa barionica di un'ammasso, può essere studiato
tramite osservazioni in banda X e sfruttando l'effetto Sunyaev-Zel'dovich
(SZ). L'effetto SZ è una distorsione dello spettro della radiazione
cosmica di fondo (CMB) causato dallo scattering Compton inverso dei fotoni
CMB all'interazione con gli elettroni caldi nell'ICM. Inoltre, l'effetto
SZ e' proporzionale alla pressione degli elettroni integrata e quindi ci
permette non solo una misura dell'energia termica degli ammassi ma anche
del loro stato morfologico.
Lo scopo di questa tesi è di studiare la struttura di un ammasso di
galassie attraverso l'effetto SZ usando dati di ALMA (RXCJ1347, Kitayama et
al. 2016) per modellare la sua morfologia. Nello specifico, sarà condotta
la riduzione dei dati, la costruzione di modelli di emissione dell'ammasso
e il confronto coi dati. Qualora i resultati su
RXCJ1347 e il tempo a disposizione lo consentano, sara' possibile
considerarne l'applicazione anche ai dati ALMA proprietari non ancora
pubblicati.
Questa tesi e' ottima per chi vuole imparare a trattare dati
interferometrici e richiede un investimento di tempo di minimo 6 mesi.

'''Contatti: Sandra Burkutean burkutean@ira.inaf.it, Marcella Massardi massardi@ira.inaf.it'''

'''Referente UniBO: Myriam Gitti'''

*'''Titolo: Giant molecular clouds properties along the bar of NGC3627'''
ALMA has the ability to resolve star-forming structures
in nearby galaxies with unprecedented sensitivity.
Detailed studies of Giant molecular clouds (GMC) previously possible only in
the Milky Way can be now done on GMC in nearby galaxies.
ALMA observations of two CO transitions (CO(1-0) and CO(2-1))
have been recently taken in the bar region of NGC3627
NGC3627 is a nearby, face-on, galaxy, with a prominent bar structure,
well observed at different frequencies.
The spatial resolution achieved at 230 GHz (CO(2-1)) is of ~30 pc.
It is possible to conduct a detailed study of the properties
of GMC in different environments: the nucleus of the galaxy,
the bar regions, the ends of the bar, the inner rings.

Lavoro:
Calibrazione e imaging dei dati ALMA.
Analisi dei dati e estrazione delle proprieta' delle GMCs.

Durata: > 6 mesi

'''Referente IRA-ARC: Rosita Paladino (paladino@ira.inaf.it)'''

'''Referente UniBO: Cristian Vignali'''

*'''Title: Unveiling the nature of high-redshift radio galaxies in the radio and millimeter band.'''

Scientific Rationale:
High-redshift radio galaxies (HzRGs) are among the most massive galaxies in the early
Universe. They have traditionally been identified by the ultra-steep spectrum of their easily detectable radio continuum, which served as a beacon for tracing
the faint host galaxy environment. HzRGs have been observed to be the signposts of large overdensities in the early Universe, the
so-called protoclusters that are believed to be the ancestors of local rich clusters. There are strong evidences that HzRGs in the center of high-z clusters are the
probable progenitor of the local Brightest Cluster Galaxies. HzRGs are therefore an ideal tool for probing the formation of
BCGs and the AGN activity in the host galaxies in premordial cluster environment.

Goals:
Clarifying the still unknown continuum millimeter and puzzling radio properties of a sample of HzRGs in the Southern Hemisphere: identification of source components (core, jets, lobes) and possibly the emission mechanisms (thermal or non-thermal?).
Studying the cold molecular gas content which is the raw ingredient for star formation and potential fuel for the AGN: how does it relate with the radio morphology?

Methods:
Analysis of archival ALMA millimeter observations, and VLA/ATCA radio data.

Acquired skills:
Archive mining, CASA imaging, analysis tools (python scripts, KAFE software)
Depending on the available time, ALMA data calibration processes

Required working time: > 6 months

'''IRA-ARC Referent: Elisabetta Liuzzo (liuzzo@ira.inaf.it)'''--
'''UniBO Referent: Myriam Gitti'''

*'''Title: The origin of the mini-starburst in the War-and-Peace Nebula'''

Aim:
To look for signs of cloud-cloud collisions in one of the
most active SF complexes in our Galaxy. This region, aka NGC6357,
contains 3 very massive open clusters, hosting some of the most
massive stars known to exist. The formation of these star clusters
may have been triggered by the collision of two or more molecular
clouds. The effects of this should be visible in the morphology and
kinematics of the molecular gas.

Available material:
maps of the entire complex in:
12CO(3-2) and 13CO(3-2) (JCMT);
Near-IR (JHK,H2) (UKIRT);
mid-IR (GLIMPSE);
dust-continuum emission (450mum, 850mum: SCUBA2; Herschel Hi-GAL)

Duration: 6 months

'''Supervisors:'''

'''IRA-ARC: Jan Brand (brand@ira.inaf.it), Andrea Giannetti (agianne@ira.inaf.it)'''

'''Arcetri: Fabrizio Massi (fmassi@arcetri.astro.it)'''

*'''Title: Dust polarization study of star-forming objects in the Orion filament'''

Magnetic fields are found to play an important role in filamentary shaped molecular clouds and most probably also in prestellar cores and young stellar objects. So far only very few polarimetric observations have been carried out at the high angular resolution and sensitivity necessary to capture single star-forming objects. The Laurea thesis will aim at retrieving the polarimetric properties of three young star-forming objects in the Orion filament using Archival ALMA data and relate this to the gravitational energy and outflow properties.

Lavoro:
Calibrazione e imaging di dati ALMA in polarizzazione.
Analisi dati polarizzazione, del dust continuum e dati CO (JCMT, Archive) per indagare la relazione del campo magnetico rispetto agli effetti di gravita' e outflow.

Durata: > 6 mesi

'''Referente IRA-ARC: Kazi Rygl (kazi@ira.inaf.it)'''

'''Referente UniBo: TBD'''

== On going theses ==

- '''Giovanni Sabatini ''': 'Establishing a timeline for the high-mass star formation process' PhD thesis, supervisor J. Brand, A. Giannetti, G. Giovannini

- '''Ilaria Ruffa ''': 'The AGN fueling/feedback cycle: a multi-phase study of a sample of local radio galaxies' PhD thesis, supervisors I. Prandoni, R. Laing, G. Giovannini

- '''Vincenzo Galluzzi''': 'Multi-frequency study of radio source polarimetry in millimetric bands' PhD thesis, supervisor M. Massardi, L. Gregorini

== Submitted theses ==

-''' Giovanni Sabatini ''', 'Unveiling the inner morphology and gas kinematics of NGC5135 with ALMA', 2017 Master Thesis, supervisor A. Ciamatti, C. Gruppioni, M. Massardi, F. Pozzi

- ''' Francesco Fragnito ''', 'Kinematics modelling of molecular gas in NGC 3100', 2017 Master Thesis, supervisor G. Giovannini, I. Prandoni, R. Paladino,

- ''' Matilde Mingozzi ''', 'Investigating the AGN-starburst connection in a nearby Seyfert galaxy with ALMA and multiwavelength data', 2016 Master Thesis, supervisor F. Pozzi, L. Vallini, A. Mignano.

- '''Ilaria Riuffa''': 'Multi wavelengths properties of a sample of obscured AGNs', 2016 Master Thesis,
Supervisor: C. Vignali, A. Mignano

- '''Eleonora Bianchi''': 'Observability of high density tracing molecular lines in lensed galaxies with ALMA' 2014 master thesis, supervisor M. Massardi, L. Gregorini

- '''Chiara Verdirame''': 'The core mass function in star-forming region NGC 6357', 2014 Master thesis, supervisor J. Brand, A. Giannetti [L. Gregorini]

- '''Andrea Giannetti''': 'The evolution of massive clumps in star forming regions', 2014 PhD thesis, supervisor J. Brand [L. Gregorini]

- '''Daria Dall'Olio''': 'IRAS16293-2422 as seen with ALMA: chemistry and morphology', 2013 Master thesis, supervisor J. Boissier [L. Gregorini], in collaboration with J. Brand, A. Mignano, R. Paladino

- '''Andrea Giannetti''': 'A detailed study of molecular clouds and star formation associated with the Galactic HII region G353.2+0.9', 2010 Master thesis, supervisor J. Brand [L. Gregorini]

Theses

2017-11-21T20:08:49Z

Kazi:

== Available projects ==

* '''Titolo: Una nuova epoca degli studi dell'effetto Sunyaev Zel'dovich con ALMA'''

Gli ammassi di galassie si trovano nei nodi della rete cosmica e sono le
più grandi strutture in equilibrio dinamico nell'Universo. Le attività di
merger durante la formazione di queste strutture lasciano tracce nella
morfologia del gas diffuso intra-ammasso (ICM). Questo plasma, formando la
maggior parte della massa barionica di un'ammasso, può essere studiato
tramite osservazioni in banda X e sfruttando l'effetto Sunyaev-Zel'dovich
(SZ). L'effetto SZ è una distorsione dello spettro della radiazione
cosmica di fondo (CMB) causato dallo scattering Compton inverso dei fotoni
CMB all'interazione con gli elettroni caldi nell'ICM. Inoltre, l'effetto
SZ e' proporzionale alla pressione degli elettroni integrata e quindi ci
permette non solo una misura dell'energia termica degli ammassi ma anche
del loro stato morfologico.
Lo scopo di questa tesi è di studiare la struttura di un ammasso di
galassie attraverso l'effetto SZ usando dati di ALMA (RXCJ1347, Kitayama et
al. 2016) per modellare la sua morfologia. Nello specifico, sarà condotta
la riduzione dei dati, la costruzione di modelli di emissione dell'ammasso
e il confronto coi dati. Qualora i resultati su
RXCJ1347 e il tempo a disposizione lo consentano, sara' possibile
considerarne l'applicazione anche ai dati ALMA proprietari non ancora
pubblicati.
Questa tesi e' ottima per chi vuole imparare a trattare dati
interferometrici e richiede un investimento di tempo di minimo 6 mesi.

'''Contatti: Sandra Burkutean burkutean@ira.inaf.it, Marcella Massardi massardi@ira.inaf.it'''

'''Referente UniBO: Myriam Gitti'''

*'''Titolo: Giant molecular clouds properties along the bar of NGC3627'''
ALMA has the ability to resolve star-forming structures
in nearby galaxies with unprecedented sensitivity.
Detailed studies of Giant molecular clouds (GMC) previously possible only in
the Milky Way can be now done on GMC in nearby galaxies.
ALMA observations of two CO transitions (CO(1-0) and CO(2-1))
have been recently taken in the bar region of NGC3627
NGC3627 is a nearby, face-on, galaxy, with a prominent bar structure,
well observed at different frequencies.
The spatial resolution achieved at 230 GHz (CO(2-1)) is of ~30 pc.
It is possible to conduct a detailed study of the properties
of GMC in different environments: the nucleus of the galaxy,
the bar regions, the ends of the bar, the inner rings.

Lavoro:
Calibrazione e imaging dei dati ALMA.
Analisi dei dati e estrazione delle proprieta' delle GMCs.

Durata: > 6 mesi

'''Referente IRA-ARC: Rosita Paladino (paladino@ira.inaf.it)'''

'''Referente UniBO: Cristian Vignali'''

*'''Title: Unveiling the nature of high-redshift radio galaxies in the radio and millimeter band.'''

Scientific Rationale:
High-redshift radio galaxies (HzRGs) are among the most massive galaxies in the early
Universe. They have traditionally been identified by the ultra-steep spectrum of their easily detectable radio continuum, which served as a beacon for tracing
the faint host galaxy environment. HzRGs have been observed to be the signposts of large overdensities in the early Universe, the
so-called protoclusters that are believed to be the ancestors of local rich clusters. There are strong evidences that HzRGs in the center of high-z clusters are the
probable progenitor of the local Brightest Cluster Galaxies. HzRGs are therefore an ideal tool for probing the formation of
BCGs and the AGN activity in the host galaxies in premordial cluster environment.

Goals:
Clarifying the still unknown continuum millimeter and puzzling radio properties of a sample of HzRGs in the Southern Hemisphere: identification of source components (core, jets, lobes) and possibly the emission mechanisms (thermal or non-thermal?).
Studying the cold molecular gas content which is the raw ingredient for star formation and potential fuel for the AGN: how does it relate with the radio morphology?

Methods:
Analysis of archival ALMA millimeter observations, and VLA/ATCA radio data.

Acquired skills:
Archive mining, CASA imaging, analysis tools (python scripts, KAFE software)
Depending on the available time, ALMA data calibration processes

Required working time: > 6 months

'''IRA-ARC Referent: Elisabetta Liuzzo (liuzzo@ira.inaf.it)'''--
'''UniBO Referent: Myriam Gitti'''

*'''Title: The origin of the mini-starburst in the War-and-Peace Nebula'''

Aim:
To look for signs of cloud-cloud collisions in one of the
most active SF complexes in our Galaxy. This region, aka NGC6357,
contains 3 very massive open clusters, hosting some of the most
massive stars known to exist. The formation of these star clusters
may have been triggered by the collision of two or more molecular
clouds. The effects of this should be visible in the morphology and
kinematics of the molecular gas.

Available material:
maps of the entire complex in:
12CO(3-2) and 13CO(3-2) (JCMT);
Near-IR (JHK,H2) (UKIRT);
mid-IR (GLIMPSE);
dust-continuum emission (450mum, 850mum: SCUBA2; Herschel Hi-GAL)

Duration: 6 months

'''Supervisors:'''

'''IRA-ARC: Jan Brand (brand@ira.inaf.it), Andrea Giannetti (agianne@ira.inaf.it)'''

'''Arcetri: Fabrizio Massi (fmassi@arcetri.astro.it)'''

*'''Title: Dust polarization study of star-forming objects in the Orion filament'''

Magnetic fields are found to play an important role in filamentary shaped molecular clouds and most probably also in prestellar cores and young stellar objects. So far only very few polarimetric observations have been carried out at the high angular resolution and sensitivity necessary to capture single star-forming objects. The Laurea thesis will aim at retrieving the polarimetric properties of three young star-forming objects in the Orion filament using Archival ALMA data and relate this to the gravitational energy and outflow properties.

Lavoro:
Calibrazione e imaging di dati ALMA in polarizzazione.
Analisi dati polarizzazione, del dust continuum e dati CO (JCMT, Archive) per indagare la relazione del campo magnetico rispetto agli effetti di gravita' e outflow.

Durata: > 6 mesi

'''Referente IRA-ARC: Kazi Rygl'''

'''Referente UniBo: TBD'''

== On going theses ==

- '''Giovanni Sabatini ''': 'Establishing a timeline for the high-mass star formation process' PhD thesis, supervisor J. Brand, A. Giannetti, G. Giovannini

- '''Ilaria Ruffa ''': 'The AGN fueling/feedback cycle: a multi-phase study of a sample of local radio galaxies' PhD thesis, supervisors I. Prandoni, R. Laing, G. Giovannini

- '''Vincenzo Galluzzi''': 'Multi-frequency study of radio source polarimetry in millimetric bands' PhD thesis, supervisor M. Massardi, L. Gregorini

== Submitted theses ==

-''' Giovanni Sabatini ''', 'Unveiling the inner morphology and gas kinematics of NGC5135 with ALMA', 2017 Master Thesis, supervisor A. Ciamatti, C. Gruppioni, M. Massardi, F. Pozzi

- ''' Francesco Fragnito ''', 'Kinematics modelling of molecular gas in NGC 3100', 2017 Master Thesis, supervisor G. Giovannini, I. Prandoni, R. Paladino,

- ''' Matilde Mingozzi ''', 'Investigating the AGN-starburst connection in a nearby Seyfert galaxy with ALMA and multiwavelength data', 2016 Master Thesis, supervisor F. Pozzi, L. Vallini, A. Mignano.

- '''Ilaria Riuffa''': 'Multi wavelengths properties of a sample of obscured AGNs', 2016 Master Thesis,
Supervisor: C. Vignali, A. Mignano

- '''Eleonora Bianchi''': 'Observability of high density tracing molecular lines in lensed galaxies with ALMA' 2014 master thesis, supervisor M. Massardi, L. Gregorini

- '''Chiara Verdirame''': 'The core mass function in star-forming region NGC 6357', 2014 Master thesis, supervisor J. Brand, A. Giannetti [L. Gregorini]

- '''Andrea Giannetti''': 'The evolution of massive clumps in star forming regions', 2014 PhD thesis, supervisor J. Brand [L. Gregorini]

- '''Daria Dall'Olio''': 'IRAS16293-2422 as seen with ALMA: chemistry and morphology', 2013 Master thesis, supervisor J. Boissier [L. Gregorini], in collaboration with J. Brand, A. Mignano, R. Paladino

- '''Andrea Giannetti''': 'A detailed study of molecular clouds and star formation associated with the Galactic HII region G353.2+0.9', 2010 Master thesis, supervisor J. Brand [L. Gregorini]

Theses

2017-11-21T19:46:03Z

Kazi: /* Available projects */

== Available projects ==

* '''Titolo: Una nuova epoca degli studi dell'effetto Sunyaev Zel'dovich con ALMA'''

Gli ammassi di galassie si trovano nei nodi della rete cosmica e sono le
più grandi strutture in equilibrio dinamico nell'Universo. Le attività di
merger durante la formazione di queste strutture lasciano tracce nella
morfologia del gas diffuso intra-ammasso (ICM). Questo plasma, formando la
maggior parte della massa barionica di un'ammasso, può essere studiato
tramite osservazioni in banda X e sfruttando l'effetto Sunyaev-Zel'dovich
(SZ). L'effetto SZ è una distorsione dello spettro della radiazione
cosmica di fondo (CMB) causato dallo scattering Compton inverso dei fotoni
CMB all'interazione con gli elettroni caldi nell'ICM. Inoltre, l'effetto
SZ e' proporzionale alla pressione degli elettroni integrata e quindi ci
permette non solo una misura dell'energia termica degli ammassi ma anche
del loro stato morfologico.
Lo scopo di questa tesi è di studiare la struttura di un ammasso di
galassie attraverso l'effetto SZ usando dati di ALMA (RXCJ1347, Kitayama et
al. 2016) per modellare la sua morfologia. Nello specifico, sarà condotta
la riduzione dei dati, la costruzione di modelli di emissione dell'ammasso
e il confronto coi dati. Qualora i resultati su
RXCJ1347 e il tempo a disposizione lo consentano, sara' possibile
considerarne l'applicazione anche ai dati ALMA proprietari non ancora
pubblicati.
Questa tesi e' ottima per chi vuole imparare a trattare dati
interferometrici e richiede un investimento di tempo di minimo 6 mesi.

'''Contatti: Sandra Burkutean burkutean@ira.inaf.it, Marcella Massardi massardi@ira.inaf.it'''

'''Referente UniBO: Myriam Gitti'''

*'''Titolo: Giant molecular clouds properties along the bar of NGC3627'''
ALMA has the ability to resolve star-forming structures
in nearby galaxies with unprecedented sensitivity.
Detailed studies of Giant molecular clouds (GMC) previously possible only in
the Milky Way can be now done on GMC in nearby galaxies.
ALMA observations of two CO transitions (CO(1-0) and CO(2-1))
have been recently taken in the bar region of NGC3627
NGC3627 is a nearby, face-on, galaxy, with a prominent bar structure,
well observed at different frequencies.
The spatial resolution achieved at 230 GHz (CO(2-1)) is of ~30 pc.
It is possible to conduct a detailed study of the properties
of GMC in different environments: the nucleus of the galaxy,
the bar regions, the ends of the bar, the inner rings.

Lavoro:
Calibrazione e imaging dei dati ALMA.
Analisi dei dati e estrazione delle proprieta' delle GMCs.

Durata: > 6 mesi

'''Referente IRA-ARC: Rosita Paladino (paladino@ira.inaf.it)'''

'''Referente UniBO: Cristian Vignali'''

*'''Title: Unveiling the nature of high-redshift radio galaxies in the radio and millimeter band.'''

Scientific Rationale:
High-redshift radio galaxies (HzRGs) are among the most massive galaxies in the early
Universe. They have traditionally been identified by the ultra-steep spectrum of their easily detectable radio continuum, which served as a beacon for tracing
the faint host galaxy environment. HzRGs have been observed to be the signposts of large overdensities in the early Universe, the
so-called protoclusters that are believed to be the ancestors of local rich clusters. There are strong evidences that HzRGs in the center of high-z clusters are the
probable progenitor of the local Brightest Cluster Galaxies. HzRGs are therefore an ideal tool for probing the formation of
BCGs and the AGN activity in the host galaxies in premordial cluster environment.

Goals:
Clarifying the still unknown continuum millimeter and puzzling radio properties of a sample of HzRGs in the Southern Hemisphere: identification of source components (core, jets, lobes) and possibly the emission mechanisms (thermal or non-thermal?).
Studying the cold molecular gas content which is the raw ingredient for star formation and potential fuel for the AGN: how does it relate with the radio morphology?

Methods:
Analysis of archival ALMA millimeter observations, and VLA/ATCA radio data.

Acquired skills:
Archive mining, CASA imaging, analysis tools (python scripts, KAFE software)
Depending on the available time, ALMA data calibration processes

Required working time: > 6 months

'''IRA-ARC Referent: Elisabetta Liuzzo (liuzzo@ira.inaf.it)'''--
'''UniBO Referent: Myriam Gitti'''

*'''Title: The origin of the mini-starburst in the War-and-Peace Nebula'''

Aim:
To look for signs of cloud-cloud collisions in one of the
most active SF complexes in our Galaxy. This region, aka NGC6357,
contains 3 very massive open clusters, hosting some of the most
massive stars known to exist. The formation of these star clusters
may have been triggered by the collision of two or more molecular
clouds. The effects of this should be visible in the morphology and
kinematics of the molecular gas.

Available material:
maps of the entire complex in:
12CO(3-2) and 13CO(3-2) (JCMT);
Near-IR (JHK,H2) (UKIRT);
mid-IR (GLIMPSE);
dust-continuum emission (450mum, 850mum: SCUBA2; Herschel Hi-GAL)

Duration: 6 months

'''Supervisors:'''

'''IRA-ARC: Jan Brand (brand@ira.inaf.it), Andrea Giannetti (agianne@ira.inaf.it)'''

'''Arcetri: Fabrizio Massi (fmassi@arcetri.astro.it)'''

*'''Title: Dust polarization study of star-forming objects in the Orion filament'''

Magnetic fields are found to play an important role in filamentary shaped molecular clouds and most probably also in prestellar cores and young stellar objects. So far only very few polarimetric observations have been carried out at the high angular resolution and sensitivity necessary to capture the single star-forming objects. The Laurea thesis will aim at retrieving the polarimetric properties of a three young star-forming objects in the Orion filament using Archival ALMA data and relate this to the gravitational energy and outflow properties.

Lavoro:
Calibrazione e imaging di dati ALMA in polarizzazione.
Analisi dati polarizzazione, del dust continuum e dati CO (JCMT, Archive) per indagare la relazione del campo magnetico rispetto agli effetti di gravita' e outflow

Durata: > 6 mesi

== On going theses ==

- '''Giovanni Sabatini ''': 'Establishing a timeline for the high-mass star formation process' PhD thesis, supervisor J. Brand, A. Giannetti, G. Giovannini

- '''Ilaria Ruffa ''': 'The AGN fueling/feedback cycle: a multi-phase study of a sample of local radio galaxies' PhD thesis, supervisors I. Prandoni, R. Laing, G. Giovannini

- '''Vincenzo Galluzzi''': 'Multi-frequency study of radio source polarimetry in millimetric bands' PhD thesis, supervisor M. Massardi, L. Gregorini

== Submitted theses ==

-''' Giovanni Sabatini ''', 'Unveiling the inner morphology and gas kinematics of NGC5135 with ALMA', 2017 Master Thesis, supervisor A. Ciamatti, C. Gruppioni, M. Massardi, F. Pozzi

- ''' Francesco Fragnito ''', 'Kinematics modelling of molecular gas in NGC 3100', 2017 Master Thesis, supervisor G. Giovannini, I. Prandoni, R. Paladino,

- ''' Matilde Mingozzi ''', 'Investigating the AGN-starburst connection in a nearby Seyfert galaxy with ALMA and multiwavelength data', 2016 Master Thesis, supervisor F. Pozzi, L. Vallini, A. Mignano.

- '''Ilaria Riuffa''': 'Multi wavelengths properties of a sample of obscured AGNs', 2016 Master Thesis,
Supervisor: C. Vignali, A. Mignano

- '''Eleonora Bianchi''': 'Observability of high density tracing molecular lines in lensed galaxies with ALMA' 2014 master thesis, supervisor M. Massardi, L. Gregorini

- '''Chiara Verdirame''': 'The core mass function in star-forming region NGC 6357', 2014 Master thesis, supervisor J. Brand, A. Giannetti [L. Gregorini]

- '''Andrea Giannetti''': 'The evolution of massive clumps in star forming regions', 2014 PhD thesis, supervisor J. Brand [L. Gregorini]

- '''Daria Dall'Olio''': 'IRAS16293-2422 as seen with ALMA: chemistry and morphology', 2013 Master thesis, supervisor J. Boissier [L. Gregorini], in collaboration with J. Brand, A. Mignano, R. Paladino

- '''Andrea Giannetti''': 'A detailed study of molecular clouds and star formation associated with the Galactic HII region G353.2+0.9', 2010 Master thesis, supervisor J. Brand [L. Gregorini]

File:Bandpass interference.png

2017-02-24T12:12:51Z

Kazi:

File:Absline bpass.png

2017-02-24T12:12:27Z

Kazi:

File:Absline phasecal.png

2017-02-24T12:11:52Z

Kazi:

File:Almachem.pdf

2016-05-24T12:39:12Z

Kazi:

File:Weblog.pdf

2016-02-10T16:51:23Z

Kazi: