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What it's about- Newborn City, NY, is a growing urban escape, created after the Dawning, where humans and demons live together in semi-harmony. Built over the foundations of the small town Endwell, Newborn City is host to every type of creature. But something evil lurks inside its alleys and dark corners, waiting to take control of the city's inhabitants. Working to stop what would surely be the beginning of the end, Newborn City's hottest, fiercest warriors struggle to defeat the most horrifying monster anyone has ever faced.
Burn the Bone- Getting feedback from betas.
General outlining of the series, which includes several LGBTQIA+ characters, way too many types of mythological creatures, and the formation of an epic battle
A Kingdom in Collapse Duet- Book One The Falling Kingdom
When her country, her kingdom, is under attack from unknown demonic forces, Atalia watches as her floating home begins to collapse on itself and sink into the clouds.
Everything is going to crumble to the ground if they don't return the Clockwork Crown.
Against safety and sense, her mother offers to fly her back to the floating castle. Once there, things only get worse. Enemies are after the Crown, and it can't leave the castle if they hope to keep it afloat.
But they can't keep it there hidden without a protector, and Atalia can't allow herself to be captured. That's when the Beast is created out of an act of love.
General concept, loose worldbuilding
Monster Romance, High Fantasy
Steampunk vibes
Novel, duet
Upcoming Co-Write with Victoria Johnson
Yes, I'm being very mysterious about this one, but I can tell you that it's set here in Vegas. It's super dark, super sexy, and super violent. It'll be one wild ride from start to not-so-finish because, of course, it's planned as a series.
His Black Alchemy
A dark high fantasy why-choose romance with orcs, fae, violence, magic, alchemy, and all the tropes! This was a result of a pick-my-tropes filter, which included academic rivals, second-chance romance, fated mates, and arranged marriage.
This one has an official blurb-
Sheyrah
I've had it up to here dealing with the King's endless obsession with pitting the fae alchemists of Hiviba against each other. I've already lost the love of my life to the Orc Kingdom Gukar when he defected, and now I'm just supposed to be his sharpened tool to create a tenuous peace? I'm not his child or relative, but I'm just supposed to marry the Gukarian King's alchemist like it's nothing. We've constantly battled, albeit mentally, about who's the better practitioner, and I'm to wed him in three days.
Sindren
The fae captain of the guard in an orc kingdom has little in the way of friends. I've never been treated the same as a less-than-magical member of the Folk, but the Orc Dynasty has perfected the art of burying emotions that don't serve you. In three days, I'm on a new assignment as the sole protector of the renowned Black Alchemist. In three days, I'll see her again.
I had little choice but to accept my fate when the Emperor informed me I would be marrying Hiviba's fae Alchemist. We've constantly sparred over the years, and the infuriating Witchling is now supposed to be my Chosen. In three days, I'll see her face for the first time, and the thought of spelling her into silence on the spot is more than tempting.
In three days, Sheyrah, Zelig, and Sindren will meet. In three days, the realm will have two powerful alchemists aligned. And in three days, the fate of all will change as a riptide of chaos roars through the planes, threatening to destroy the Radiance that gives life to magic.
The first four parts are available on Patreon!
Dreaming of Electric Sheep
The leader of the Resistance has been kidnapped by the corrupt people running things. Still, instead of simply imprisoning her or letting her mind go to waste, she is forced into a coma where she's convinced she's just a lowly tech employee. Until she gets the message in her mind that it's been 20 long years and she must wake up.
General outlining and character planning, this is a raw shell right now, but it demanded my attention.
Progress is being made in worldbuilding
Cyberpunk/Neon Sci-Fi
Throuple Romance
Sins of the Innocent– Lovely Little Hell Trilogy
Join Mallory and her men in Sins of the Innocent. When Mallory Jenkins finds a strange sigil carved into the floor of her attic, she does a little digging- literally. When she finds that she is, in fact, the result of necromancy gone a bit wrong, she must confront her summoner, her mother, and a Death God who is none too pleased that she skipped out on him. As she progresses through the layers of the Underworld, Mallory meets the men, nay the Gods, that each owns a part of her soul. She needs the pieces to be whole again, but maybe that doesn't mean they can't own them too.
Filled with tempting dark Gods and Loa, blood, a psychic cat, and enough bones to make a warlock blush, Sins of the Innocent is sure to be a fantastic trip through the small town of Hallows End, LA.
Why Choose/Polyam Romance with Horror, Southern Gothic Aesthetic
Novel- potential trilogy
Outlining, rambles, character development
Through a Hawk's Eyes
Arrow and Grey don't want to work together, but when the entire world as they know it is crumbling around them in shards of etherium, they do what they must. In a dark high-fantasy-style tale, two completely different individuals find that connection and intimacy occur at the most inconvenient times. When a Nothing threatens the world, magick sparks to life in unlikely places, and the past comes a-knocking, quite literally. This pair of warriors find that life is more than just swords and sorcery.
General outlining and character planning, which includes a lot of development work for my bisexual demisexual lady and her bisexual demiromantic beau
So much worldbuilding
Dark High Fantasy Romance
They had always called me the Red Queen, and the name fit. I was oft-covered in the crimson blood of those I vanquished and devoured.
Writing and expanding on previous sections
Violence, sex, and lots of blood
Sapphic vampires with a very dom-sub dynamic
Dark Vampire Fantasy Romance
This one has a blurb now as well-
𝐈𝐧 𝐭𝐡𝐢𝐬 𝐬𝐩𝐢𝐜𝐲 𝐫𝐞𝐭𝐞𝐥𝐥𝐢𝐧𝐠 𝐨𝐟 𝐀𝐥𝐢𝐜𝐞 𝐢𝐧 𝐖𝐨𝐧𝐝𝐞𝐫𝐥𝐚𝐧𝐝, 𝐲𝐨𝐮'𝐥𝐥 𝐟𝐨𝐥𝐥𝐨𝐰 𝐭𝐡𝐞 𝐰𝐢𝐧𝐝𝐢𝐧𝐠 𝐩𝐚𝐭𝐡 𝐝𝐨𝐰𝐧 𝐢𝐧𝐭𝐨 𝐝𝐚𝐫𝐤𝐧𝐞𝐬𝐬 𝐰𝐢𝐭𝐡 𝐀𝐥𝐢𝐜𝐞 𝐚𝐬 𝐬𝐡𝐞 𝐟𝐚𝐥𝐥𝐬 𝐩𝐫𝐞𝐲 𝐭𝐨 𝐭𝐡𝐞 𝐑𝐞𝐝 𝐐𝐮𝐞𝐞𝐧. 𝐀 𝐛𝐥𝐨𝐨𝐝𝐭𝐡𝐢𝐫𝐬𝐭𝐲 𝐜𝐫𝐞𝐚𝐭𝐮𝐫𝐞 𝐭𝐡𝐚𝐭 𝐞𝐱𝐜𝐢𝐭𝐞𝐬 𝐚𝐧𝐝 𝐭𝐞𝐫𝐫𝐢𝐟𝐢𝐞𝐬 𝐀𝐥𝐢𝐜𝐞, 𝐡𝐨𝐥𝐝𝐢𝐧𝐠 𝐩𝐫𝐨𝐦𝐢𝐬𝐞𝐬 𝐨𝐟 𝐫𝐞𝐯𝐞𝐧𝐠𝐞, 𝐥𝐮𝐬𝐭, 𝐚𝐧𝐝 𝐩𝐨𝐰𝐞𝐫.
How far down the rabbit hole will she fall?
FF/Sapphic
Dual POV
Pararnormal Vampire Romance
Morally Grey MCs
Violence/Blood/Gore
Fem Dom/Sub
DubCon
Praise/Deg
Blood Play
Knife Play
Tragic Pasts
Mention of Prior Abuse
The Red Queen is a vampire fantasy retelling of Alice in Wonderland. A dark erotic fantasy romance for sure! The Red Queen is an ancient being who Alice finds herself compelled to seek out. Alice falls down the rabbit hole as she becomes the Red Queen's new favored companion and learns what it's like to be a creature who feasts on others, just like her beloved Queen.
The first three parts are available now on Kindle Vella!


Career Сenter is part of the Kazakh National Pedagogical University named after Abai and operates under the Charter KazNPU named after Abai. The activities of the Center is to assist students in apprenticeship and the maximum possible employment of university graduates.
- prediction of the structure of demand in the labor market based on an analysis of the labor market, determining the supply and demand of specialists in regional and professional qualification section.
- monitors the degree of satisfaction of employerslevel of knowledge of graduates.


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Fraudulent Biden Admin
Update: Biden Announces Sweeping Executive Order to Advance Radical "LGBTQI+" Agenda In Schools – New EO Bans "Conversion Therapy," Which Now Includes 'Suggesting' That a Child Should Not Undergo Medical Transition
Posted BY: Julian Conradson
It's 2022 and up is down, the sky is purple, gas prices are sprinting towards $10, Monkeypox is bigoted, and now executive orders are being used to groom your kids. Welcome to hell Joe Biden's America.
On Wednesday, Joe Biden announced that he would be signing another executive order to bolster the left's radical gender identity crusade in schools across America.
The sweeping EO will provide funding to the Department of Education in order to create a new advocacy group that "issues guidance" on LGBTQI+ policies to "states, school districts, and other educational institutions," and also sends resources to the Department of Health and Human Services (HHS) that would focus on gender identity affirmation services for students in the US.
One of the main goals of the new legislation will be to expand access to destructive "gender-affirming" drugs and medical procedures for children despite mounting evidence of the severe long-term consequences (sterility, bone loss, other health issues) and increased suicide rates among young people who are coerced into medically transitioning.
Trending: The Communist Plot behind School Shootings
Thanks to a few researchers who are finally doing the work and looking into this issue, the results are becoming crystal clear – 'gender-affirming care,' which entails pumping children full of puberty blockers and cross-sex hormones, is making the problem measurably worse.
But, it shouldn't take a scientist or a clinical study to see that we should not be giving young children, who don't have the faculties to make these types of life-altering decisions on their own, drugs that are used to chemically castrate pedophiles (Lupron, puberty blocker) – let alone giving young, healthy girls' double mastectomies in the name of 'gender affirmation' – it's unspeakable what these monsters are doing to America's children.
And now, Biden is mandating this poison with a stroke of a pen.
From the WH announcement and "fact sheet":
"Today, to mark Pride Month, President Biden will sign an Executive Order Advancing Equality for LGBTQI+ Individuals…
…Order charges HHS to work with states to promote expanded access to gender-affirming care…
…[the EO] directs the Department of Education to establish a new Working Group on LGBTQI+ Students and Families, which will advance policies for states, school districts, and other educational institutions to promote safe and inclusive learning environments in which all students thrive…"
In addition to providing resources to expand the Federal Governments LGBTQAI+ push, the order would also ban "conversion therapy" – which is defined by Merriam Webster as: "the use of any of various methods (such as aversive stimulation or religious counseling) in an attempt to change a person's sexual orientation to heterosexual or to change a person's gender identity to correspond to the sex the person has."
However, under the new EO, the definition of "conversion therapy" was expanded widely. Now, simply suggesting that a child refrains from undergoing medical procedures to change their gender will be classified as such, and, therefore, would be effectively outlawed once Biden signs the order, according to the Post Millennial. Failing to affirm the child's gender wishes in any way could result in consequences for school officials, child counselors, and even medical professionals who receive federal funding of any sort.
As if the grooming problem in schools wasn't bad enough already…
From the Post Millennial:
"It was only recently, during the Transgender Visibility Day, that Biden told parents across America to "affirm" their children, meaning that should a child claim to be what they are not, parents should nod affirmatively and sign them up for irrevocable courses of medical treatment that will prevent them from living full lives.
Filled with rhetoric and emotional flourishes, this new order states that so-called conversion therapy must be banned across the country, but it warps the language of conversion therapy to say that for youth who identify as transgender, it would be a therapeutic conversion to suggest to them that they not alter their healthy bodies to match their gender dysphoria.
Biden also declares in this executive order that federally-funded programs cannot offer so-called 'conversion therapy.'" This means that children who present as transgender must be affirmed to be transgender and cannot be cautioned off of that course. He intends to prevent conversation therapy globally with this EO as well."
Biden's EO goes directly against state's rights and forces the adoption of these unspeakable medical practices and destructive ideologies nationwide. Several states, such as Texas and Florida, have enacted laws that protect children from these 'gender-affirming' procedures and defend the reality of biological sex – which is apparently a bridge too far for the Biden Regime.
According to the WH announcement, this sweeping order comes, in part, because of "over 300 anti-LGBTQI+ laws" that have been introduced in Republican-led states "over the past year." Unbelievably, the "fact sheet" baselessly alleges that these laws "specifically target" trans children and are effectively a form of "hateful" bullying on the part of said state legislatures.
However, despite having so many instances of 'outright bigotry' to choose from, no specific examples were provided to back up their bogus anti-LGBTQI+ claims.
From the WH:
"Over 300 anti-LGBTQI+ laws have been introduced in state legislatures over the past year, and many of them specifically target transgender children and their parents by banning access to medical care and support at school. President Biden is addressing these harmful, hateful, and discriminatory attacks head-on – not only by speaking up for America's families, but taking action to stand up to the bullies targeting LGBTQI+ people."
With Biden's latest EO, it's official – add 'grooming' to the Build Back Better agenda.
Biden Announces Sweeping Executive OrderUS News
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redpajama_set_name: RedPajamaCommonCrawl


Well, it has been a very interesting week for schools throughout the area and state. With the recent weather, we can state it is "one for the record books"! I hope that you and your family were able to be safe and stay warm during the week. We were excited to see our students as they returned to school today.
There are many different ways to describe last week's weather which caused schools to be closed for four days. ISD 197 was very cooperative in notifying us of their decisions to cancel school. Keeping our students, families, and faculty safe during these unusual circumstances is a priority. I have requested the ISD 197 district administration keep me informed of their discussions and decisions regarding rescheduling (making up) any school days missed during this week. I will make decisions regarding making up / rescheduling school days based upon the information provided by the school district.
When describing St. Joseph's School, many people refer to it as a "family". You are important members of our school family! Your commitment to provide a Catholic education for your children is shared by the members of this family. The important relationships between the home and the school, parents and faculty, students and teachers, and parish and school are evident in our school family. The support you offer your children and our faculty makes this a very special and blessed school.
As our school plans for the 2019-2020 school year, I want to thank you for continuing to be an important member of the St. Joseph's School family. The faculty and I thank you for entrusting your children to us each day. It is a privilege to partner with you to provide them with strong faith formation and quality learning experiences. Let's pray together that, "God's will be done" for our families and school.
Neither snow, nor wind, nor cold, nor school being cancelled will prevent us from celebrating our school and Catholic Schools Week. Our celebrations will be held next week, February 4-8. I invite your children and family to participate in the activities. Our celebration will include special themes days, Mass, and Carnival. Updated information may be found in the Important Links section of this letter. We hope that you are able to join us for the celebration.
Unfortunately, due to scheduling constraints, our Fan Appreciation Week will not be able to be rescheduled. However, plans are being finalized for our Cheer Squad to cheer at games in the near future.
An article written by Archbishop Bernard Hebda on the value of Catholic Schools is included in the January 24, 2019 edition of the Catholic Spirit (the Archdiocesan Newspaper). Archbishop Hebda writes; "We are blessed in this archdiocese to have not only a strong tradition of vibrant youth ministry and religious education, but also a deeply rooted commitment to excellent Catholic schools, continuing the work that began when the Sisters of St. Joseph opened the first Catholic school for our local Church in 1851." The entire article and the Roadmap for Excellence in Catholic Education may be found in that edition of the Catholic Spirit.
Parent Teacher Conferences are scheduled for Tuesday, February 5 (4:30-7:30 pm) and Thursday, February 7 (4:30-7:30 pm). Conferences will be held in our classrooms. Either the teacher or the parent may request a conference to discuss a student's progress. CLICK HERE to schedule your conference.
Mid-trimester Progress Reports for students in grades 4-8 were mailed to families this week. Please schedule a conference with your child's teacher(s) if you have questions or need additional information about your child's progress at school.
Congratulations to our second grade students who received their First Reconciliation on Saturday, January 26. The students attended a special retreat and received the sacrament with their families. We thank Fr. Creagan, Fr. Wratkowski, Mrs. Fallon, Mrs. Taplin, and our families for preparing the students to receive this special sacrament. Please continue to pray for the students as they prepare to receive Jesus at their First Holy Communion on Saturday, April 27.
We would like to thank everyone for attending the Catholic Schools Week Mass at the Church of St. Joseph and our Open House in our school. We thank Mrs. Bowe and our middle school choir for providing the music. We thank Mrs. Frost, members of our School Advisory Council, and our school faculty for welcoming the visitors to our school. Thank you for celebrating and supporting our school.
Our annual school Carnival will now be held on Friday, February 8, 2019 from 12:00 noon-3:00 p.m. Our Carnival Committee is looking for several volunteers to help during Carnival. Please CLICK HERE to volunteer! In addition, the Committee is looking for prizes of all kinds for the General Store and items for the popular Raffle. Prizes may be brought to the school office. Please CLICK HERE to sign up to donate. Thank you for your assistance and support of the special event for our students.
Kindergarten Information Session – Thank you!
We would like to thank the many families who attended the Kindergarten Information Session this week. The administration, faculty, and staff shared information about our school's Kindergarten program. The families also toured our Kindergarten classrooms and the Level I Atrium during the evening. Anyone who was not able to attend the information night is invited to call the school office to set up an appointment for a visit and tour of our school.
Current school families with children in grades K-7 have been automatically re-enrolled for next school year. The annual family registration fee ($200/family) will be applied to family TADS accounts in February. Families may visit the Admissions page on our website for 2019-2020 school tuition information. For questions about enrollment, contact Christy Frost at 651-789-8315 or chfrost@stjosephwsp.org.
We always invite and encourage our families to share information about our school with your families, neighbors, and friends. A $500 Referral Credit is available to current school families for each new family they refer which registers to attend our school for next year. Thank you for your assistance and sharing our school story.
St. Joe's STEM Fair – April 4, 2019 *Please note date change from prior letter.
Calling all scientists, engineers, mathematicians, and inventors! All students in grades 3-8 are invited to participate in St. Joseph's School first ever STEM Fair. STEM stands for Science, Technology, Engineering, and Mathematics. Winners of the St. Joe's STEM Fair will be able to compete in the CSCOE Big Bang STEM Fair on April 6, 2019. Due to the weather and to allow our students time to complete their projects, the St. Joe's STEM Fair has been rescheduled to Thursday, April 4, 2019. Middle School Science and Engineering Teacher, Miss Schafer, will be in all the classrooms, grades 3-8, to explain all the details to students in the next couple of days. A STEM Fair information packet may be found in the Important Links section of this letter. Please print out the information at home and go over it with your child. If you child is interested in participating in this special academic event, please complete the St. Joseph's School STEM Fair Registration Form and return. If you have any questions, please email elschafer@stjosephwsp.org.
We need help for recess duty for the remaining months of school. Whether our students are outside or inside because of the weather, volunteers offer tremendous assistance in providing supervision of students. Please look for an email from your grade level rep and consider signing up for recess duty.
The Scholastic Book Fair will be held in our Library next week! We need Volunteers to assist with this event. Please CLICK HERE to sign up!
Students in grades K – 5 will be going to the Library to preview the Book Fair on Tuesday, February 5 with their class. Students will bring home a wish list with items that they are interested in purchasing at the fair. Thursday, February 7 will be their Book Fair purchase day. If you are interested in purchasing items from your students wish list or other items, please send money to school with your student.
The Scholastic Book Fair will be open during Parent Teacher Conferences 4:00pm-8:00pm on Tuesday, February 5 and Thursday, February 7. It will also be open at Church in the Great Room on Saturday, February 9 - 5:30pm - 6:30pm, and Sunday, February 10 - 8:30am - 12:00pm. Please contact the school office if you have any questions about this year's Book Fair.
School families are invited to the next St. Joseph's School Family Night at Panera in West St. Paul. This special community event will be on Wednesday, February 13 between 4:00pm and 8:00pm. Come enjoy a delicious meal and great fellowship with school families and friends. Please bring in the Panera flyer or show an electronic version (see attached) for our school to receive a percentage of your purchase.
Please join us for our school Mass on Friday, February 8 at 9:00am in the church. School families, friends, and members of the parish are always invited to pray with our students and faculty.
Parents are asked to please stop and check the tables with items from our lost and found during Parent Teacher Conferences. The table will be located on the second floor of our building near the school office. There are many items including coats, hats, gloves, shoes, and gym bags. Thank you for checking and claiming any of your items.
The annual Church of St. Joseph Father – Daughter Dance is scheduled for February 8. The dance will be held in the Church's Great Room from 6:30-9:30-pm. This event is open to all ages. Please watch the parish bulletin for ticket information. If you are interested in helping with this event, please contact Tracy Kracht at 651-457-2709 or ryan_kracht@msn.com.
We are all called to holiness. Learning about the universal call to holiness is the first of four parts of our parish mission. Everyone is invited to learn how personal holiness is at the core of welcoming the stranger. Please see the parish website https://churchofstjoseph.org/ for more information and to register for the mission.
St. Joseph's will be hosting an All in God's Plan Level 1 event for 10-12 years old girls and their mothers or significant adult female on Saturday, March 9, 2019 from 2-4:30pm. Space will be limited. Please see the parish website for registration details.
St. Joseph's Catholic School educates students through faith formation, academic excellence, and the development of virtue to be disciples of Christ.
Click here to link to the weekly St. Joseph's Church Bulletin .


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Bauhaus Museum in Tel Aviv
The White City of Tel Aviv, UNESCO World Cultural Heritage Site since 2003, adds to its vast collection of International Style buildings a new Bauhaus Museum,…
Aqua-Scape in Japan
Here you take a tour around the portable architecture object; it was set up in a pool and is used by children as a place to play.
The Prada Art Foundation model unveiled
The Office for Metropolitan Architecture OMA unveiled their plans for the new Prada Art Foundation. A tower by Rem Koolhaas, which will be integrated in an…
City & Countryside
Olympia Buildings Beijing
Photogallery about the Buildings for Olympia 2008 in Beijing.
Page 271 of 283.


Based on consultation with company MORIS we have offered solution by extraction unit FT 650 LZ which has waste container with emptying to central extraction system. The FT 650 LZ is connected to the CNC as individual extractor and the emptying pipe is connected to the current central extraction system. The total extraction capacity increased and while there is still no need of waste manipulation.
The project from first visit, through project, production and assemlby of the unit was finished within 4 weeks.
We would like to thank to MORIS design and their staff for co-operation and we will be looking forward to farther projects.


text:
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Kicking the Can Down the Road: Government Interventions in the European Banking Sector
69 Pages Posted: 14 Oct 2018
See all articles by Viral V. Acharya
Viral V. Acharya
New York University - Leonard N. Stern School of Business; Centre for Economic Policy Research (CEPR); National Bureau of Economic Research (NBER); New York University (NYU) - Department of Finance
Sascha Steffen
Frankfurt School of Finance & Management
Lea Borchert
ZEW – Leibniz Centre for European Economic Research; University of Mannheim; Frankfurt School of Finance & Management
Date Written: September 22, 2018
Building on a novel and comprehensive dataset of all government interventions in the eurozone banking sector, we analyze the implications of government interventions in the European banking sector during the 2007 to 2009 financial crisis for the subsequent sovereign debt crisis. We find that governments with weaker public finances were more reluctant to recapitalize distressed banks during the financial crisis of 2007 to 2009. Insufficient recapitalizations of distressed banks had significant negative consequences for financial stability and real sector lending as weak banks remained vulnerable to future shocks, increased their risk-taking and did not write down defaulted loans by evergreening loans to "zombie" borrowers.
Keywords: regulatory forbearance; evergreening; zombie lending; sovereign debt crisis; bank recapitalization; fiscal constraints; political economy
JEL Classification: E44, G21, G28, G32, G34
Suggested Citation: Suggested Citation
Acharya, Viral V. and Steffen, Sascha and Borchert, Lea, Kicking the Can Down the Road: Government Interventions in the European Banking Sector (September 22, 2018). Available at SSRN: https://ssrn.com/abstract=3253517 or http://dx.doi.org/10.2139/ssrn.3253517
New York University - Leonard N. Stern School of Business ( email )
44 West 4th Street
New York, NY NY 10012
HOME PAGE: http://pages.stern.nyu.edu/~sternfin/vacharya/public_html/~vacharya.htm
Centre for Economic Policy Research (CEPR)
New York University (NYU) - Department of Finance
Stern School of Business
Sascha Steffen (Contact Author)
Frankfurt School of Finance & Management ( email )
Adickesallee
Frankfurt, 60322
16097326929 (Phone)
HOME PAGE: http://www.sascha-steffen.de
ZEW – Leibniz Centre for European Economic Research ( email )
L 7,1
Mannheim, 68161
+49 0621 1235-311 (Phone)
University of Mannheim ( email )
L9, 1-2
Adickesallee 32-34
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\section{Introduction}
\label{intro}

X-ray emission is a characteristic footprint of active galactic nuclei (AGN), and it is known to vary at short and long timescales. In some cases, the origin of X-ray variability in AGN could be attributed to the passage of intervening material across our line of sight. This situation is of particular interest as it can be useful to probe the dynamics and physical properties of the matter in the vicinity of the central supermassive black hole (SMBH). Such situations have been reported for the case of short eclipses, possibly due to the passing of broad line region clouds (NGC 1365, \citealt{Ris07}; Mrk 766, \citealt{Ris11}), and for longer periods, as in NGC 5548, where a long-lived stream of matter is obscuring the central source for several years (\citealt{Kaa14}). In fact, the systematic study of \citet{Mar14} shows that this kind of obscuration event may happen recurrently in a majority of AGN but they may pass unnoticed due to the lack of continuous monitoring.

NGC 985 (also known as Mrk 1048), may be another case of a recorded eclipsing event. It is a nearby $z = 0.043$~(\citealt{Fis95}) Seyfert 1 galaxy which shows a distinctive ring-shaped structure, testimony of a recent merger event. NGC 985 also shows a persistent outflow in both the X-ray and the UV, revealed by a multi-component warm absorber (WA) in the X-ray, and blue-shifted absorption troughs in both wavebands (\citealt{Arav02a}; \citealt{Kro05,Kro09}). Following a {\sl Swift}{} monitoring programme, NGC 985 was discovered to be in a low soft X-ray flux state in July 2013, which triggered a joint XMM-{\sl Newton}{} and HST observation (\citealt{Par14}). We recently observed NGC 985 using both XMM-{\sl Newton}{} and the Hubble Space Telescope (HST) in an effort to monitor the time variability of the persistent absorbers and thereby determine their density, distance, mass flux, and kinetic luminosity. Our observations in January 2015 show that the source is back to an overall high X-ray flux state, and therefore emerging from an absorption event. This work is organized as follows: in Sect.~\ref{observations} we describe the observations used and the data reduction methods, in Sect.~\ref{sed} we derive the spectral energy distribution of NGC 985, in Sect.~\ref{results} we report the data analysis, and in Sect.~\ref{discussion} we discuss the results and summarize our findings. We adopt a cosmological framework  with $H_{\rm 0} = 70$~km s$^{-1}$~Mpc$^{-1}$, $\Omega_{\rm M} = 0.3$, and $\Omega_{\Lambda} = 0.7$. The quoted errors refer to 68.3\% confidence level ($\Delta \chi^2 = 1$~for one parameter of interest) unless otherwise stated.

\section{Observations}
\label{observations}

NGC 985 has been observed by XMM-{\sl Newton}{} in five occasions: once in 2003, and twice in 2013 and 2015. The first observation of 2013 (ObsID 0690870101) was too short ($\sim$20~ks of exposure time) and was excluded from this analysis. The rest of the observations, summarized in Table~\ref{xmmlog}, were retrieved from the XMM-{\sl Newton}{}~Science Archive (XSA\footnote{{\tt http://xmm.esac.esa.int/xsa/}}) and re-processed using SAS v14.0. The spectra taken with EPIC-pn, which was operated in Small Window mode to prevent pile-up, were extracted using the {\tt xmmselect} task. The source extraction region was a 40 arcsec radius circle centered at the boresight coordinates; the background was extracted using a region of the same size positioned in an area of the detector devoid of X-ray sources. After filtering from background flaring, the EPIC-pn net exposure times were those listed in Table~\ref{xmmlog}.

We observed NGC 985 with the Cosmic Origins Spectrograph (COS) on the Hubble Space Telescope (HST) in two visits coordinated with the most recent XMM-{\sl Newton}{} observations. We also retrieved a previous COS observation from the Mikulski Archive for Space Telescopes (MAST\footnote{{\tt https://archive.stsci.edu}}) which was coordinated with the prior XMM-{\sl Newton}{} observation of \citet{Par14}. Table \ref{HSTObsTbl} gives the details of the data sets from the multiple observations. The far-ultraviolet (FUV) channel of COS nominally covers a wavelength range of 1150--1775 \AA\ with a resolving power of $\sim$18,000 (\citealt{Gre12}). Our observations in January 2015 as well as the archival observations from 2013 used gratings G130M and G160M to span these wavelengths. At the redshift of NGC 985, prominent lines such as Ly$\alpha$, \ion{N}{v}, \ion{Si}{iv}, \ion{C}{iv}, and \ion{He}{ii} appear in our spectra. More recently commissioned modes of COS extend wavelength coverage to as short as the Lyman limit at 912 \AA. Our 2015 observations used grating G140L and a central wavelength setting of 1280 to also cover 1000--2000 \AA~at a resolving power of $\sim2000$, which allows us to view the Ly$\beta$ and \ion{O}{vi} transitions in NGC 985. All observations used multiple central wavelength settings and focal-plane positions (FP-POS) to allow our merged spectra to span the gaps between the two detector segments and eliminate flat-field features and detector defects. The individual exposures were combined with updated wavelength calibrations, flat-field procedures, and flux calibrations as described by \citet{Kriss11b} and \citet{DeR15}. The wavelength zero point was adjusted by matching the low-ionization interstellar absorption features in the spectrum to the \ion{H}{i} velocity of $v_{LSR}=-7~\rm km~s^{-1}$ (\citealt{Wak11}).

   \begin{table}
     \centering
     \caption[]{XMM-{\sl Newton}{}~observations log of NGC 985.}
     \label{xmmlog}
     %
     \begin{tabular}{l c c c}
       \hline\hline
       \noalign{\smallskip}
       ObsID & Obs. Date & Exp. Time & Net Exp. Time \\
              &  (yyyy-mm-dd) & (ks) &    (ks) \\
       \noalign{\smallskip}
       \hline
       \noalign{\smallskip}
       0150470601 & 2003-07-16 & 57.9 & 31.7\\
       0690870501 & 2013-08-10 & 103.7 & 71.6  \\
       0743830501 & 2015-01-13 & 138.9 & 94.0 \\
       0743830601 & 2015-01-25 & 122.0 & 72.0 \\
       \noalign{\smallskip}
       \hline
     \end{tabular}
   \end{table}

\begin{table*}
  \centering
  \caption[]{HST/COS observations of NGC 985}
\label{HSTObsTbl}
\begin{tabular}{l c c c c c}
\hline\hline
\noalign{\smallskip}
Proposal ID & Data Set Name & Grating/Tilt  & Date & Start Time (UT) & Exposure (s)\\
\noalign{\smallskip}
\hline
\noalign{\smallskip}
12953 & lbz801010 & G130M/1327 & 2013-08-12 & 13:04:43 & $\phantom{0}$851 \\
12953 & lbz801020 & G130M/1309 & 2013-08-12 & 13:24:31 & $\phantom{0}$850 \\
12953 & lbz801030 & G160M/1577 & 2013-08-12 & 14:41:47 & 1145 \\
12953 & lbz80040q & G160M/1600 & 2013-08-12 & 16:06:00 & 1141 \\
\noalign{\smallskip}
\hline
\noalign{\smallskip}
13821 & lcjm01010 & G130M/1291 & 2015-01-14 & 02:39:32 & $\phantom{0}$600 \\
13821 & lcjm01020 & G130M/1309 & 2015-01-14 & 02:52:52 & $\phantom{0}$600 \\
13821 & lcjm01030 & G130M/1327 & 2015-01-14 & 03:06:12 & 1505 \\
13821 & lcjm01040 & G160M/1577 & 2015-01-14 & 04:21:22 & 1430 \\
13821 & lcjm01050 & G160M/1611 & 2015-01-14 & 05:37:27 & $\phantom{0}$775   \\
13821 & lcjm01060 & G160M/1600 & 2015-01-14 & 05:53:30 & $\phantom{0}$775   \\
13821 & lcjm01070 & G160M/1589 & 2015-01-14 & 06:09:33 & $\phantom{0}$775   \\
13821 & lcjm01080 & G140L/1280 & 2015-01-14 & 07:13:00 & 5161 \\
13821 & lcjm02010 & G130M/1291 & 2015-01-26 & 02:43:45 & $\phantom{0}$600 \\
13821 & lcjm02020 & G130M/1309 & 2015-01-26 & 02:57:05 & $\phantom{0}$600 \\
13821 & lcjm02030 & G130M/1327 & 2015-01-26 & 03:10:25 & 1505 \\
13821 & lcjm02040 & G160M/1577 & 2015-01-26 & 04:25:14 & 1430 \\
13821 & lcjm02050 & G160M/1611 & 2015-01-26 & 05:41:18 & $\phantom{0}$775  \\
13821 & lcjm02060 & G160M/1600 & 2015-01-26 & 05:57:21 & $\phantom{0}$775  \\
13821 & lcjm02070 & G160M/1589 & 2015-01-26 & 06:13:24 & $\phantom{0}$775 \\
13821 & lcjm02080 & G140L/1280 & 2015-01-26 & 07:16:50 & 5161 \\
\noalign{\smallskip}
\hline
\end{tabular}
\end{table*}

\section{Spectral energy distributions}
\label{sed}

We constructed the spectral energy distributions (SED) of the observations using the contemporaneous measurements of XMM-{\sl Newton}{}~EPIC-pn in X-rays, HST in the UV (except for the 2003 observation in which no contemporaneous HST data were available), and the XMM-{\sl Newton}{}~optical monitor (OM) in the UV/optical. The X-ray SED was obtained from the best-fit EPIC-pn model (see Sect.~\ref{xrays}) corrected from instrinsic and Galactic absorption. In the UV we used the HST-COS continuum fluxes at 1175, 1339, 1510, and 1765~\AA~corrected for Galactic extinction using the reddening curve prescription of \citet{Car89}, assuming a color excess $E(B-V)=0.03$~mag based on calculations of \citet{Sch98} as updated by \citet{Sch11}, as given in the NASA/IPAC Extragalactic Database (NED), and a ratio of total to selective extinction $R_{\rm V} \equiv A_{\rm V}/E(B-V)$ fixed to 3.1. The OM observations were taken with the $V$, $B$, $U$, $UVW1$, $UVM2$, and $UVW2$ filters in the 2013 and 2015 observations, except for the 2003 observation, in which only $U$, $UVW1$, $UVM2$, and $UVW2$ filters were used. The OM fluxes were also corrected for Galactic extinction using the reddening curve of \citet{Car89}, including the update in the optical/near-IR of \citet{Don94}. To correct for the host galaxy starlight contribution in the OM filters we used the bulge galaxy template of \citet{Kin96}, scaled to the host galaxy flux at the rest-frame wavelength $F_{\rm gal, 5100 \AA} = 2.48 \times 10^{-15}$~erg cm$^{-2}$~s$^{-1}$~\AA$^{-1}$ (\citealt{Kim08}). The adopted SEDs are shown in Fig.~\ref{sedfig}.

\begin{figure}
  \centering
  \hbox{
  \includegraphics[width=6cm,angle=-90]{sed_all.ps}
  }
  \caption{\label{sedfig}Spectral energy distributions of the 2015a (solid line), 2015b (dashed line), 2013 (dot-dashed line), and 2003 (dotted line) observations. The bands covered by HST-COS and XMM-{\sl Newton}{}~are also indicated.}
\end{figure}

\section{Results}
\label{results}

\subsection{X-rays}
\label{xrays}

The EPIC-pn spectra were analyzed using the {\tt SPEX}\footnote{{\tt http://www.sron.nl/spex}} fitting package (\citealt{Kaa96}) version 2.06.01. The fitting method employed was $\chi^2$ statistics. We adopted a cosmological redshift for NGC 985 of $z = 0.043$~(\citealt{Fis95}). The foreground Galactic column density was set to $N_{\rm H} = 3.17 \times 10^{20}$~cm$^{-2}$~(\citealt{Kal05}) using the {\it hot} model in SPEX, with the temperature fixed to 0.5 eV to mimic a neutral gas. Throughout the analysis we assumed proto-Solar abundances of \citet{LP09}. The spectra were fitted in the $0.3-10$~keV range, and the data were binned using the optimal binning command {\it obin}.

The continuum of the EPIC-pn spectra was modeled in the same way for all the observations. A power-law model provides an unacceptable fit in all the cases: reduced $\chi^2_\nu \sim 25$ for 234 and 236 degrees of freedom in the 2015 observations, $\chi^2_\nu \sim 14$ for 219 degrees of freedom in the 2013 observation, and $\chi^2_\nu \sim 6$ for 221 degrees of freedom in the 2003 observation. There were positive and negative residuals in the soft X-ray band, signatures of intrinsic absorption and a soft excess. The latter was modeled using a modified black body ({\it mbb} model in SPEX), which takes into account modifications of a simple black body model by coherent Compton scattering based on the calculations of \citet{KB89}. The addition of this component improved the fit by $\Delta \chi^2/\Delta \nu = 420/2$, $1875/2$, $3197/2$, and $3734/2$ in the 2003, 2013, and both 2015 observations, respectively. Interestingly, a single power law did not render a good fit of the overall continuum, even if we took into account the effects of intrinsic absorption (see below), showing a persistent hard excess above the Fe K region, particularly significant in the 2015 observations. A broken power-law model was used instead, improving the overall continuum fit and rendering a very significant improvement of the fit of $\Delta \chi^2/\Delta \nu = 168/2$, and $232/2$ in the two 2015 observations, respectively. This effect is less evident, but still significant, in the 2003 and 2013 observations, with $\Delta \chi^2/\Delta \nu = 11/2$, and $8/2$, respectively. The Fe K$\alpha$ line was modeled with a Gaussian line, whose parameters did not vary significantly between observations, thus indicating an origin in matter distant from the central SMBH. In addition, the 2003 pn spectrum shows a small emission line at $\sim 8.8$~keV, which is attributed to a Cu instrumental feature. Its presence was also reported in \citet{Par14}, and it has no impact in the results and conclusions presented in this paper.

\begin{figure}
  \centering
  \hbox{
  \includegraphics[width=7cm,angle=-90]{pn_all.ps}
  }
  \caption{\label{pnfig}XMM-{\sl Newton}{}~EPIC-pn spectra of NGC 985 in 2003, 2013, and 2015. The solid grey line represents the best-fit model.}
\end{figure}

\begin{table*}
  \centering
  \caption[]{Best-fit results of the XMM-{\sl Newton}{}~EPIC-pn spectra of NGC 985.}
  \label{xtab}
  %
  \renewcommand\arraystretch{1.1}
  \begin{tabular}{l|l c c c c}
    \hline\hline
    \noalign{\smallskip}
    Model  &  Parameter &  Obs. 2003  &  Obs. 2013  &  Obs. 2015a  &  Obs. 2015b \\
    \noalign{\smallskip}
    \hline
    \noalign{\smallskip}
    Power-law & ${\rm F_{(0.3-10~keV)}}$\tablefootmark{a} & $1.11^{+0.12}_{-0.08} \times 10^{-11}$ & $8.79^{+0.64}_{-0.42} \times 10^{-12}$ & $2.02^{+0.12}_{-0.06} \times 10^{-11}$ & $2.93^{+0.06}_{-0.04} \times 10^{-11}$ \\
             & $\Gamma$\tablefootmark{b} & $2.21^{+0.09}_{-0.03}$ & $1.71^{+0.07}_{-0.03}$ & $2.14 \pm 0.02$ & $2.22 \pm 0.02$ \\
             & $E_{\rm 0}$\tablefootmark{c} &  $3.72^{+0.19}_{-0.96}$  &  $2.69 \pm 0.15$ & $4.54 \pm 0.17$ & $3.54 \pm 0.07$ \\
             & $\Delta\Gamma$\tablefootmark{d} &  $-0.37 \pm 0.07$  & $-0.19^{+0.05}_{-0.07}$ & $-0.42 \pm 0.02$ & $-0.37 \pm 0.02$ \\
    \noalign{\smallskip}
    \hline
    \noalign{\smallskip}
    Mod. BB  & ${\rm F_{(0.3-10~keV)}}$\tablefootmark{a} & $2.7^{+0.8}_{-0.2} \times 10^{-12}$ & $9.3 \pm 1.6 \times 10^{-13}$ & $1.7 \pm 0.1 \times 10^{-12}$ & $2.5 \pm 0.2 \times 10^{-12}$ \\
             & $T$\tablefootmark{e} & $0.232 \pm 0.007$ & $0.211 \pm 0.004$ & $0.160 \pm 0.005$ & $0.146 \pm 0.003$ \\
    \noalign{\smallskip}
    \hline
    \noalign{\smallskip}
    Gauss    & ${\rm F_{line}}$\tablefootmark{a} & $2.4 \pm 0.3 \times 10^{-13}$ & $1.8 \pm 0.2 \times 10^{-13}$ & $1.9 \pm 0.2 \times 10^{-13}$ & $1.5 \pm 0.2 \times 10^{-13}$ \\
             & $E$\tablefootmark{f} & $6.48 \pm 0.02$ & $6.47 \pm 0.02$ & $6.50 \pm 0.01$ & $6.47 \pm 0.02$ \\
             & FWHM\tablefootmark{g} & $0.39 \pm 0.06$ & $0.22 \pm 0.04$ & $0.28 \pm 0.04$ & $0.21 \pm 0.05$ \\
    \noalign{\smallskip}
    \hline
    \noalign{\smallskip}
   {\it xabs} 1  & $\log \xi$\tablefootmark{h} & $2.84 \pm 0.03$ & $2.86 \pm 0.03$ & $2.81 \pm 0.01$ & $2.78 \pm 0.02$ \\
             & $N_{\rm H}$\tablefootmark{i} & $7.2^{+5.2}_{-4.0} \times 10^{22}$ & $2.1 \pm 1.0 \times 10^{22}$ & $9.8^{+2.8}_{-1.8} \times 10^{22}$ & $2.4 \pm 0.3 \times 10^{22}$\\
    \noalign{\smallskip}
    \hline
    \noalign{\smallskip}
   {\it xabs} 2  & $\log \xi$\tablefootmark{h} & $1.88 \pm 0.02$ & $1.83 \pm 0.06$ & $2.03 \pm 0.02$ & $2.18 \pm 0.09$ \\
             & $N_{\rm H}$\tablefootmark{i} & $1.8 \pm 0.2 \times 10^{22}$ & $1.0 \pm 0.3 \times 10^{22}$ & $8.8 \pm 0.8 \times 10^{21}$ & $4.6^{+1.1}_{-0.5} \times 10^{21}$ \\
    \noalign{\smallskip}
    \hline
    \noalign{\smallskip}
    {\it xabs} 3  & $\log \xi$\tablefootmark{h} & $\dots$ & $1.58^{+0.12}_{-0.21}$ & $1.29 \pm 0.12$ & $1.80 \pm 0.05$ \\
             & $N_{\rm H}$\tablefootmark{i} & $\dots$ & $4.0^{+1.4}_{-3.0} \times 10^{21}$ & $1.3 \pm 0.4 \times 10^{21}$ & $4.0^{+0.9}_{-0.3} \times 10^{21}$ \\
    \noalign{\smallskip}
    \hline
    \noalign{\smallskip}
    {\it xabs} 4  & $\log \xi$\tablefootmark{h} & $-1.29 \pm 0.12$ & $-0.94 \pm 0.13$ & $-0.84 \pm 0.24$ & $-0.55^{+0.90}_{-0.30}$ \\
   (Obscurer)    & $N_{\rm H}$\tablefootmark{i} & $1.4^{+0.2}_{-0.5} \times 10^{22}$ & $2.1 \pm 0.2 \times 10^{22}$ & $5.5^{+1.2}_{-0.5} \times 10^{21}$ & $7.0^{+1.2}_{-2.1} \times 10^{21}$ \\
             & $f_{\rm C}$\tablefootmark{j} & $0.85^{+0.02}_{-0.18}$ & $0.92 \pm 0.01$ & $0.30 \pm 0.04$ & $0.18 \pm 0.03$ \\
    \noalign{\smallskip}
    \hline
    \noalign{\smallskip}
    $\chi^2$/d.o.f. &  &  $200/212$ & $262/208$ & $300/223$ & $298/225$ \\
    \noalign{\smallskip}
    \hline
  \end{tabular}
  \tablefoot{
    \tablefoottext{a}{Observed flux, in units of erg cm s$^{-1}$;}
    \tablefoottext{b}{Power-law photon index, corresponds to the slope of the low-energy branch;}
    \tablefoottext{c}{Power-law energy break, in units of keV;}
    \tablefoottext{d}{Power-law photon index break, corresponds to the slope of the high-energy branch of the spectrum when substracted from $\Gamma$;}
    \tablefoottext{e}{Modified black body temperature, in units of keV;}
    \tablefoottext{f}{Line energy, in units of keV;}
    \tablefoottext{g}{Line FWHM, in units of keV;}
    \tablefoottext{h}{Ionization parameter, in units of erg cm s$^{-1}$;}
    \tablefoottext{i}{Hydrogen column density, in units of cm$^{-2}$;}
    \tablefoottext{j}{Covering factor.}
    }
\end{table*}

Absorption caused by ionized gas was modeled using the {\it xabs} model, which calculates the transmission of a slab of material where all the ionic column densities are linked through a photoionization balance model computed with CLOUDY version 13.01 (\citealt{Fer13}), using as inputs the SED of NGC 985 described in Sect.~\ref{sed}. We used as free parameters in this model the hydrogen column density $N_{\rm H}$ and the ionization parameter, defined as $\log \xi = L/nR^2$, where $L$ is the ionizing luminosity in the $1-1000$~Ryd range, $n$ is the density of the gas, and $R$ is the distance to the central ionizing source. The addition of a single {\it xabs} component significantly improved the fit ($\Delta \chi^2/\Delta \nu = 477/2$, $572/2$, $1861/2$, and $2236/2$ in the 2003, 2013, and both 2015 observations, respectively.), although several absorption residuals remained in the soft X-ray range of the spectra. A second WA was therefore added, further improving the fit by $\Delta \chi^2/\Delta \nu = 12/2$, $71/2$, $265/2$, and $310/2$. The presence of some residuals below $\sim$1.5~keV in the 2015 observations motivated the inclusion of an additional WA ($\Delta \chi^2/\Delta \nu = 84/2$, and $63/2$). The 2013 observation allowed also for this extra component ($\Delta \chi^2/\Delta \nu = 77/2$), but its addition to the model in the 2003 observation no longer improved the fit. These WAs have ionization parameters ranging from $\log \xi \sim 1.3$ to $\sim 2.8$, and column densities in the range of $N_{\rm H} \sim 10^{21}$~to a few times $10^{22}$~cm$^{-2}$.

Furthermore, we modeled the transient obscuration seen in the 2013 observation with a neutral absorber, fixing the ionization parameter to $\log \xi \equiv -4$, leaving the column density $N_{\rm H}$ and covering factor as free parameters (\citealt{Par14}). This improved the overall fit by $\Delta \chi^2/\Delta \nu = 131/2$ but it left absorption residuals at $\sim 1$~keV. A much better fit, however, was obtained when we set the ionization parameter free ($\Delta \chi^2/\Delta \nu = 18/1$), indicating that this obscuration is not caused by fully neutral matter but by a mildly ionized gas ($\log \xi = -0.94 \pm 0.13$) with $N_{\rm H} = 2.1 \pm 0.2 \times 10^{22}$ and high covering factor ($0.92 \pm 0.01$). This component was the ultimate cause of the low soft X-ray flux state. Interestingly, the 2015 spectra required some of this additional absorption, $\Delta \chi^2/\Delta \nu = 20/3$, and $15/2$, albeit with a much lower covering factor, in line with the results of the contemporaneous HST-COS observations (see Sect.~\ref{uv}). The 2003 observation also required this additional very low ionization obscurer ($\Delta \chi^2/\Delta \nu = 57/3$), in a somewhat intermediate state between the 2013 and 2015 observations. We note that due to the resolution of EPIC-pn it is very difficult to appropriately constrain all the WA parameters involved in this fit. Some of them, like the outflow velocity of the intervening gas, can only be modeled through the analysis of high-resolution spectra. We stress, however, that the presence of a multi-component WA is significantly required to obtain a good fit to the data. A detailed analysis of the WA in NGC 985 using the RGS spectra of these observations will be reported in a forthcoming paper (Ebrero et al., in preparation). The best-fit results are reported in Table~\ref{xtab}, and the different EPIC-pn spectra are shown in Fig.~\ref{pnfig}.

\subsection{UV}
\label{uv}

Our HST observations of NGC 985 show the usual bright, blue continuum and broad emission lines typical of Seyfert 1 galaxies with an overall appearance similar to all prior UV observations of this object. The six components of the persistent UV absorption enumerated by \citet{Arav02a} are prominent in all three epochs of COS spectra. The most surprising new feature, however, is highly blue-shifted broad absorption that appears for the first time in 2013, and shows some residual traces in Ly$\alpha$ in our 2015 spectra.

We first noticed the potential Ly$\alpha$ absorption feature in our 2015 COS observations. We eliminated the possibilitiy that this was merely an instrumental artifact by examining the individual spectra acquired at different central wavelength settings and focal-plane positions. The feature appeared in all individual spectra in both observations. We also checked the white dwarf spectra acquired each month to monitor the sensitivity variations in COS (\citealt{Hol14}). The Ly$\alpha$ feature does not appear in any of the preceding or following monitor spectra. Finally, we examined the archival spectra of NGC 985 from 2013, where we saw the much stronger Ly$\alpha$ absorption as well as the troughs from several other ions.

Figure \ref{HSTspectra} compares the COS spectrum from 2013, when the heavy X-ray obscuration was present, to the average spectrum from our two observations in 2015, when the low-energy X-ray absorption had dissipated. The 2015 spectrum shown in Figure \ref{HSTspectra} is a time-weighted average of the individual exposures obtained in our two visits. NGC 985 varied slightly in flux between the two visits. On 2015-01-14, the continuum flux was $\rm F_\lambda(1410) = 4.1 \times 10^{-14}~ergs~cm^{-2}~s^{-1}~\AA^{-1}$. Twelve days later, on 2015-01-26, it was $\rm F_\lambda(1410) = 4.6 \times 10^{-14}~ergs~cm^{-2}~s^{-1}~\AA^{-1}$. In the 2013 spectrum, one can see that the broad UV absorption was prominent in transitions of \ion{C}{iii}*, Ly$\alpha$, \ion{Si}{iv}, and \ion{C}{iv}, but shows only traces in Ly$\alpha$ in the 2015 spectrum. \ion{N}{v} absorption may be present in 2013, but it is difficult to measure since it falls on top of the peak of the Ly$\alpha$ emission line.

\begin{figure*}
  \centering
  \includegraphics[width=14cm, angle=-90]{fig2_091815.eps}
  \vspace{-6cm}
  \caption{Calibrated and merged COS spectrum of NGC 985 from 2013 (black) and 2015 (red). The spectrum has been binned by 8 pixels (1 resolution element) for display purposes. We indicate the most prominent emission features with black labels and tick marks; blue labels indicate the broad absorption features that are most prominent in the 2013 spectrum. An Earth symbol is atop the geocoronal Ly$\alpha$ emission line in the center of the Milky Way \ion{H}{i} absorption trough.}
  \label{HSTspectra}
\end{figure*}

To measure the characteristics of the broad UV absorption lines, we fit a multi-component model to the continuum, emission lines, and broad absorption lines that is similar to our model of NGC 5548 (\citealt{Kaa14}). We use the {\tt specfit} fitting package (\citealt{Kriss94}) to model the spectrum. For the continuum, we use a reddened power law in $f_{\lambda}$ with $\rm E(B - V) = 0.03$ (\citealt{Sch11}; \citealt{Sch98}) absorbed by foreground Galactic \ion{H}{i} with a column density of $3.17 \times 10^{20}~\rm cm^{-2}$ (\citealt{Kal05}). The emission lines are treated as multiple Gaussian emission components, and the broad absorption lines as Gaussian components in negative flux. Since the broad absorption lines are highly blue shifted, the details of the emission line profiles do not affect our measurements, and we will discuss the emission model in more detail in a future publication that discusses the narrow absorption lines. For the broad absorption troughs in the COS 2013 spectrum, free parameters include the equivalent width (EW), the velocities, and the full-width-at-half-maximum (FWHM). For \ion{C}{iv} and  \ion{Si}{iv}, the velocities of the doublets are tied together, and the widths are tied as well. Initially we forced all lines to have the same FWHM. In our final iteration, when the FWHM were permitted to vary freely, they all settled at the same best-fit value. In the 2015 spectrum, since only Ly$\alpha$ was visible, we permitted only its parameters to vary freely. For the other lines, we fixed the velocity and the FWHM at the best-fit values obtained for the 2013 spectrum in order to determine the upper limits (1-$\sigma$ confidence) on the equivalent widths. In Table \ref{AbsTbl} we give the velocities, widths, and equivalent widths of the broad absorption lines.

\begin{table*}
  \centering
  \caption[]{Properties of the Broad UV Absorption Lines in NGC 985}
  \label{AbsTbl}
\begin{tabular}{l c c c c c c}
\hline\hline
\noalign{\smallskip}
{Line} & $\lambda_o$ & {EW} & {Velocity} & {FWHM} & $\rm C_f$ & $\rm N_{ion}$\\
      & (\AA)       & (\AA) & ($\rm km~s^{-1}$) & ($\rm km~s^{-1}$) & & ($10^{14}~\rm cm^{-2}$)\\
\noalign{\smallskip}
\hline
\noalign{\smallskip}
{COS 2013} \\
\noalign{\smallskip}
\hline
\noalign{\smallskip}
\ion{C}{iii}* & 1175.67 & $1.70 \pm 0.06$ & $-6130 \pm 50$ & $1420 \pm 50$ & 0.27 & $>1.9$ \\
Ly$\alpha$ & 1215.67  & $1.30 \pm 0.04$ & $-5970 \pm 20$ & $1420 \pm 50$ & 0.21 & $>2.9$ \\
\ion{Si}{iv} & 1393.76 & $1.03 \pm 0.04$ & $-5950 \pm 20$ & $1420 \pm 50$ & 0.14 & $>2.9$ \\
\ion{Si}{iv} & 1402.77 & $0.96 \pm 0.04$ & $-5950 \pm 20$ & $1420 \pm 50$ & 0.13 & $>2.9$ \\
\ion{C}{iv} & 1548.20  & $1.00 \pm 0.04$ & $-5950 \pm 20$ & $1420 \pm 50$ & 0.13 & $>5.3$ \\
\ion{C}{iv} & 1550.77  & $0.94 \pm 0.04$ & $-5950 \pm 20$ & $1420 \pm 50$ & 0.12 & $>5.3$ \\
\noalign{\smallskip}
\hline
\noalign{\smallskip}
{COS 2015} \\
\noalign{\smallskip}
\hline
\noalign{\smallskip}
\ion{C}{iii}* & 1176.12 & $<0.14$ & $-6130$ & $1420$ & $<0.02$ & $<0.15$ \\
Ly$\alpha$ & 1215.67  & $0.26 \pm 0.04$ & $-5300 \pm 10$ & $350 \pm 50$ & $>0.11$ & $0.55$ \\
\ion{Si}{iv} & 1393.76 & $<0.08$ & $-5950$ & $1420$ & $<0.02$ & $<0.1$ \\
\ion{Si}{iv} & 1402.77 & $<0.08$ & $-5950$ & $1420$ & $<0.02$ & $<0.1$ \\
\ion{C}{iv} & 1548.20  & $<0.08$ & $-5950$ & $1420$ & $<0.02$ & $<0.1$ \\
\ion{C}{iv} & 1550.77  & $<0.08$ & $-5950$ & $1420$ & $<0.02$ & $<0.1$ \\
\noalign{\smallskip}
\hline
\end{tabular}
\end{table*}

Figure \ref{AbsNorm} shows normalized absorption profiles for these absorption lines in the 2013 COS spectrum. From the nearly equal depths of the red and blue components of \ion{Si}{iv} and \ion{C}{iv} as shown by these profiles and the equivalent widths in Table \ref{AbsTbl}, it is likely that these absorption features are saturated, and that they only partially cover the underlying emission regions. The covering fraction $\rm C_f$ given Table \ref{AbsTbl} is determined for coverage of all underlying emission components at the deepest point of each absorption trough. We have insufficient information to unambiguously determine whether the absorption primarily covers only the continuum source, or portions of both the continuum source and the broad emission-line region (BLR), but, given that there is essentially no line emission in the portion of the spectrum absorbed by \ion{C}{iii}*, and since covering fractions for the other ions are lower, it seems likely that the broad absorption we detect primarily covers the continuum emission region and only a small fraction at most of the BLR. In determining the covering fraction, we assume that each absorption line is completely saturated at the center of the trough. To determine the total column densities given in Table \ref{AbsTbl}, we integrated the normalized absorption profiles assuming the troughs represent apparent optical depth (AOD) (e.g., see \citealt{Arav02b}), but, given the high degree of saturation, we simply quote those values as lower limits.

\begin{figure}
  \centering
   \includegraphics[width=8.5cm]{ngc985_cos2015b8_broadabs_092515.eps}
  \caption{Prominent broad absorption features in the 2013 COS spectrum of NGC 985. We plot normalized relative fluxes as a function of velocity relative to the systemic redshift of $z=0.043$. The spectra have been binned by 8 pixels (1 resolution element) for display purposes. The top panel shows the \ion{C}{iii}* multiplet. The middle two panels show the \ion{Si}{iv} and \ion{C}{iv} absorption troughs with the red component of each doublet as a red line and the blue component as a blue line. The bottom panel shows the Ly$\alpha$ absorption trough. The smooth thin line in each panel shows our fit to the normalized spectrum.}
  \label{AbsNorm}
\end{figure}

The broad absorption features we detect in the COS 2013 spectrum of NGC 985 vary on approximately the same timescale as the appearance and disappearance of the sof X-ray obscuration reported by \citet{Par14}. Figure \ref{BroadAbsVary} compares the Ly$\alpha$ absorption region in all the HST archival spectra of NGC 985. In the 1999 STIS spectrum analyzed by \citet{Arav02a}, no broad Ly$\alpha$ absorption is present. The broad absorption is prominent in 2013, but it is only weakly present in our two COS spectra obtained in January 2015. For these latter two COS observations, the broad  Ly$\alpha$ absorption has diminished to a weak trough on the red wing of the absorption feature detected in the 2013 spectrum. Our 2015 observations also include short-wavelength G140L spectra that cover the Ly$\beta$ and \ion{O}{vi} regions of the NGC 985 spectrum. While we detect the typical strong \ion{O}{vi} emission line and associated narrow \ion{O}{vi} absorption, we do not see broad \ion{O}{vi} absorption nor Ly$\beta$ absorption. The non-detection of Ly$\beta$ absorption in 2015 is consistent with the Ly$\alpha$ absorption being optically thin in 2015, so in Table \ref{AbsTbl} we quote AOD column densities for the Ly$\alpha$ absorption in the 2015 spectrum, and upper limits for the other ions.

\begin{figure}
  \centering
   \includegraphics[width=7cm, angle=-90]{ngc985_lya_var_062215.eps}
  \caption{Normalized archival HST spectra of NGC 985 covering the region of Ly$\alpha$ absorption seen in the 2013 and 2015 COS spectra. The 1999 STIS spectrum is in green; the 2013 COS spectrum is in black; the 2015-01-14 COS spectrum is in blue; the 2015-01-26 COS spectrum is in red. For display purposes, the COS spectrum have been binned by 8 pixels (1 resolution element); the STIS spectrum has not been binned. Interstellar absorption features unrelated to NGC 985 are designated with a "G".}
  \label{BroadAbsVary}
\end{figure}

The six narrow absorption components identified by \citet{Arav02a} have full-widths-at-half-maximum of $\sim50~\rm km~s^{-1}$ and span a velocity range of $-810$ to $+210~\rm km~s^{-1}$. The best fit photoionization solution obtained by \citet{Arav02a} gave a total column density of $\rm log~N_H = 21.4$~cm$^{-2}$ for an ionization parameter of $\rm log~U=-0.3$ (equivalent to $\rm log~\xi \sim -1.8$ for the SED given in Sect.~\ref{sed}). In our spectra, these lines have not changed in velocity or width, and they are present only in Ly$\alpha$, Ly$\beta$, \ion{C}{iv}, \ion{N}{v} and \ion{O}{vi}. As in \citet{Arav02a}, the lines are partially saturated, particularly in neutral hydrogen, and they only partially cover the source.  The line depths vary among all four observations. From the variability timescales, we will be able to constrain the density of the absorbing gas in all six components. In concert with photoionization solutions, we will then be able to determine the distance of these absorbing components from the nuclear source. We will present this detailed analysis in a subsequent paper (Ebrero et al., in preparation).

\section{Discussion and conclusions}
\label{discussion}

\begin{figure}
  \centering
  \hbox{
  \includegraphics[width=6.5cm,angle=-90]{hr.ps}
  }
  \caption{\label{hrfig}Soft ($0.2-2$~keV) and hard ($2-10$~keV) X-ray fluxes (top and central panels, respectively), and hardness ratio (bottom panel) of NGC 985 as measured by {\sl Beppo}-SAX{} (1999), {\sl Chandra}{} (2002), and XMM-{\sl Newton}{} (2003, 2013, and 2015). Fluxes are in units of $10^{-11}$~erg cm$^{-2}$ s$^{-1}$. The dashed line represents the average hardness ratio from {\sl Swift}{} observations in 2007-2008, when the source was unobscured.}
\end{figure}

NGC 985 seems to have undergone an eclipsing event caused by mildly ionized gas crossing our line of sight. The main effect of this absorption is the decrease in the soft X-ray flux while the hard X-rays are mostly unaffected, which leads to a higher hardness ratio (HR). It is common to use HR measurements as a proxy for the detection of obscuration events (\citealt{Kaa14}). In Fig.~\ref{hrfig} we show the soft and hard X-ray fluxes, and the hardness ratio measured for NGC 985 in different observations in the last two decades. The soft X-ray flux hit a minimum in 2013, and it increases again in 2015 by more than one order of magnitude, whereas the hard X-ray flux, less prone to be affected by absorption, has varied less than a factor of 2 or 3. Indeed, the HR of NGC 985 in 2013 was much higher than in 2015 (0.66 versus $\sim 0$), but the latter values are still slightly higher than the expected HR value in the case that no obscuration is taking place, which is of the order of $-0.14$. This value is the average HR from {\sl Swift}{} observations in 2007-2008 when the source showed a persistently high soft X-ray flux, indicative that it was in an unobscured state. This would mean that in 2015 we are catching the source emerging from an absorbed state caused by intervening material but it is not yet fully unabsorbed. Furthermore, the HR in 2003 is also much higher than the unabsorbed value, also supported by the best-fit results shown in Table~\ref{xtab}. Since there were no hints of absorption in 2002, the source could be entering a similar absorbed state in 2003, which would mean that these eclipsing events are recurrent given that {\sl Swift}{} monitoring between 2007 and 2008 indicated high soft X-ray flux levels (\citealt{Par14}).

We cannot determine a precise ionization parameter or total column density for the UV absorbing gas in the 2013 COS spectrum since we merely have a set of lower limits on ionic column densities, not definitive measurements. However, we can say that the range of ions we observe (\ion{C}{iii}, \ion{Si}{iv}, and \ion{C}{iv}) are consistent with gas having an ionization parameter in the range log $\xi \sim -1.0$ to $-0.5$. Our lower limits on the column densities are also compatible with the total column density seen in the low-ionization X-ray obscurer, {\it xabs} 4. For example, if we use log $\xi=-0.94$, which corresponds to X-ray absorbing component {\it xabs} 4 in the 2013 observation, our most stringent lower limit is for \ion{Si}{iv}, for which we get $\rm N_{\rm H} > 5 \times 10^{19}$~cm$^{-2}$. Therefore, it is likely that the same gas causing the low-energy X-ray obscuration is also the gas producing the broad UV absorption lines.

We also can not establish a precise location for the broad UV absorbing gas, but the covering fractions we discussed in Sect.~\ref{results} suggest that the gas covers more of the continuum source than the BLR. Therefore, the gas is likely in or near the BLR, which is consistent with the high velocities we observed both in width and in radial motion.

The appearance of broad, high-velocity UV absorption at the same time as the strong, soft X-ray obscuration in NGC 985 strongly suggests that the obscurer is due to a wind associated with an accretion disk. This is now the third possible obscuration event detected in otherwise unobscured Seyfert 1 galaxies. The most thoroughly studied other example is the X-ray and UV obscurer that appeared in NGC 5548 (\citealt{Kaa14}), which still appears to be present. In addition, the weak \ion{C}{iv} absorption detected in Mrk 335 (\citealt{Lon13}) several months after a low-flux obscuration event is similar to the behavior we have observed in NGC 985, where we see weak UV absorption still present many months (18) after the original X-ray obscuration.

In NGC 5548, the X-ray and UV obscurer may cover as much as 100\% of the ionizing continuum (\citealt{Kaa14}); this shadowing results in a dramatic suppression of the ionizing flux that is manifested by the presence of many lower ionization absorption lines associated with the persistent, narrow UV absorption lines (\citealt{Arav15}). In NGC 985, since the UV obscuration appears not to be as deep and covering perhaps no more than 27\% of the continuum, the suppression of ionizing flux is not as dramatic. We do not see the same lowering of ionization state of the narrow UV absorbers as was observed in NGC 5548.

The sporadic nature of obscuration associated with high velocity outflows in Seyfert 1 galaxies is consistent with a picture in which the outflows are largely confined to the plane of the accretion disk, and only occasionally cross our line of sight as streamers or clumps rising chaotically from the edges of the outflow. In such a picture, broad absorption-line quasars, where such obscuration is the rule rather than the exception, would represent a class of objects viewed at higher inclination than typical Seyfert 1s. Continued monitoring of bright Seyfert 1s to trigger multiwavelength follow-up observations can yield greater insights into these phenomena.

\begin{acknowledgements}
This work is based on observations obtained by XMM-{\sl Newton}{}, an ESA science mission with instruments and contributions directly funded by ESA member states and the USA (NASA). SRON is supported financially by NWO, the Netherlands Organization for Scientific Research. This work was supported by NASA through a grant for HST program number 13812 from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. We thank the anonymous referee for his/her useful comments that helped to improve the paper.
\end{acknowledgements}

redpajama_set_name: RedPajamaArXiv


Sacred Geometry is said to be the language of the universe and the flower of life is one of the oldest symbols that was used by ancient mystics. Its earliest finding was in The Temple of Osiris in Abydos, Egypt and was also found in many homes of the early churches and synagogues in the Galilee and in Mesada. The "Flower of Life" contains the patterns of creation as they emerged from the "Great Void". Everything is made from the Creator's thought. Its symmetry is that of many circles all within a larger circle with each line touching the lines next to them. This is a symbol of unity and connectedness as one body yet many members all working together as something beautiful and unto perfection. In this interview David Hopkins speaks with TruthSeekah about his near death experience as a child and being able to access higher states of consciousness by gazing into the Flower of Life Symbol. David mentions that as he gazes into the symbol the flower of life seemed to "come alive" and become 3D leaping off of the surface that it was drawn on. There is a process of hypnosis by simply learning to draw the sacred geometric symbol similar to that of drawing Metatrons Cube. Another thing that is touched on in this episode is the aspect of spiritual awakening and how one must move past a state of psychosis when they first are aware of energies and messages from the aether realms. This is very important and and also a huge reason why The TruthSeekah Podcast is pivotal right now for people undergoing a spiritual awakening. This podcast if nothing else simply lets people know that one they are not alone and two, they are not crazy. It helps so much to simply hear those words and hear other people vocalize the experiences you've been feeling inside as well.


Hemp is trending upward, thanks to the growing popularity of the plant and its oil. It but that's not all: Many homeowners are turning to hemp as a basic material to decorate their homes with taste.
This all-natural plant fiber has become sustainable building and decorating items. It grows tightly spaced so that reduces the amount of land required for cultivation, it requires very little — if any — pesticides, it's highly renewable, and of course it absorbs CO2, so it effectively cleanses the air.
You can to make your own, or purchase them in almost any home goods store. Although hemp rope is usually brown or tan, you can dye it or paint the finished mat to achieve a desired color.
Both hemp ropes and fabric can be turned into large, as well. You might be amazed by what a talented rug artist can do with hemp-rope swirls, to create a gorgeous pattern for any room.
or old vases. Instead, refinish them with hemp rope. Wind the rope tightly around the container, and glue it in place. Add colored rope swirls and flowers to the finished product for a bit of pizzazz.
Hemp can be used to make beautiful wall decor, especially when stamped with tribal or floral patterns. You can also take colored hemp rope and let it . Use several different colors for a rainbow effect.


text:
Businesses urged to cease use of till receipts containing potentially harmful chemicals
Rachael Ridley
Planet Ark has partnered with paper specialists Alliance Paper to encourage businesses to adopt thermal paper till receipts that are better for our health and the environment.
The Queensland-based company are working with Planet Ark to put Aussie businesses on a roadmap that will eventually see all till receipts be free of chemicals of concern. The first step in the process is to raise awareness around the presence of the chemical bisphenol A (BPA) in till receipts currently used in many checkouts across Australia, and its potential health and environmental impacts.
What is BPA?
BPA is a low-cost industrial chemical used for the coatings on thermal paper (the paper that till receipts are made out of) because of its stability and heat resistance. BPA is an endocrine disruptor, meaning that it can interfere with the system in the human body that produces and manages hormones.
Handling till receipts that contain BPA can lead to absorption of the chemical through the skin. There are concerns that frequent exposure may have adverse reproductive health effects. This is particularly concerning for anyone who handles till receipts on a daily basis, such as checkout operators and retail assistants. As the chemical is not readily biodegradable, there is also concern that it could accumulate in our waterways and make its way into the food chain.
BPA was first raised as a chemical of concern in baby bottles, where it was voluntarily phased out by major Australian retailers in 2010. While there are no plans to restrict use of the chemical in till receipts in Australia, despite regulations in place in Europe*, Alliance Paper has opted to use alternatives to BPA of its own accord.
Is exposure to BPA dangerous?
Based on studies of the health effects of BPA on animals and extrapolating to humans, BPA is undoubtedly hazardous at high levels of exposure. Humans are exposed to much lower levels of BPA in their day-to-day lives, and scientific opinion is divided over what risk, if any, that level poses to humans. However, there is growing scientific evidence that even at these lower levels of exposure, BPA may be causing problems such as infertility, obesity, breast cancer, prostate cancer, heart disease and diabetes.
Planet Ark supports initiatives that limit our exposure to potentially harmful chemicals and has entered into partnership with Alliance Paper due to The Precautionary Principle, which states that "when an activity raises threats of harm to human health or the environment, precautionary measures should be taken even if some cause and effect relationships are not fully established scientifically."
If you are a business owner and want to protect your employees and customers from potentially harmful chemicals by transitioning to safer thermal paper, contact us for more information.
If you are a retail worker and are concerned about exposure to BPA through handling till receipts, ask your employer who their supplier of thermal paper is and if the paper is BPA free. You could also consider voicing your concern with your employer or manager and wearing gloves when handling till receipts.
*The European Parliament and the Council passed Regulation (EU) No. 2016/ 2235 requiring that thermal paper with a BPA concentration equal or higher than 0.02 wt% will no longer be allowed to be marketed from 2 January 2020 onwards.
Rachael joined Planet Ark in 2019 after eight years working in media and publishing as a producer, editor and writer. Rachael is excited to use her skills in content creation and communication to instigate positive environmental behaviour change.


Track: 20 CHEAP AND AWESOME CHRISTMAS GIFTS AND DIYs (Ideas gift crafts present Student squidoo homemade christmas tutorials men).
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I headed down to the waterfront for this post. A true Island girl at heart, I love featuring the ocean, so I thought this quiet fishing wharf would work. Luckily my only company included a cormorant, some passing boaters who waved hello, and wandering tourists stopped to chat. It was a beautiful island evening, with a perfect breeze off the water - lovely!
P.S. I am delighted to announce that the winner of my Joe Fresh polish giveaway is the lovely Gabrielle! Thanks to all for entering! Keep an eye out for more great giveaways coming up soon!
Gorgeous photos, gorgeous setting, gorgeous girl! I like those shoes better. ;) Love you Bec!
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You go girl! I always get nervous when people are walking around near where I am taking photos!
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THE day was chilly but die-hard Swaffham fans were warmed by a memorable 29-0 victory over hosts Haverhill.
An early penalty was awarded to Swaffham as the pack chased down Lines' start kick and forced Haverhill to illegally play the ball on the deck.
From the resulting kick to touch, a good line-out move was ended prematurely as Gladman was robbed of the ball.
Haverhill cleared their lines but the early pressure showed Swaffham's commitment to the challenge ahead.
Soon after Haverhill touched down behind their own line as a clever chip nearly saw the opening try. The first scrum was a show of Swaffham's power. Gunnell, in particular, was all over his opposite prop in the front row.
From the scrum Harris made a sensational break off the flank, scrounging the ball at the back. Bartlett was in support and received the offload from Harris, but was unfortunate to knock the ball on, under considerable pressure from the Haverhill covering defence.
The Haverhill scrum was again under pressure but nevertheless the home side won the ball and fed to their big inside-centre in an attempt to run the ball out of their 22.
He was no match for Barnard though, who created the first try with a monstrous hit on his opposite man, dislodging the ball. Harris gleefully dropped on it to bag the first try. Bartlett took the conversion in the absence of injured Steve Webb and successfully made it 7-0.
From the re-start Gunnell ran it straight back into the heart of Haverhill, the defence was good and it was only the hard work of Gunnell's support that lead to the ball retention.
Chris Hamilton also made good yards, given ball with space to run. He straightened well and Matt Taylor was on hand to secure the ball once again.
With all this possession and good territory the next score was inevitable. DJ Barnard put the pace on to go round the outside of the Haverhill defence and his super offload to J Taylor left Taylor and Bartlett two on one against the Haverhill full-back. Taylor unselfishly passed to to Bartlett, who touched down and then converted his own try for 14-0 after 15 minutes.
The score remained the same until half-time. This was mostly due to the huge Swaffham defensive effort, for a Haverhill try was on the cards.
For long periods of time Haverhill were camped out on Swaffham's five-metre line but big hits, in particular from R Gladman and L Gunnell, kept the attackers at bay. J Palmer was having a good game, marshalling his pack with confidence and conviction at scrum-half.
It was Palmer who set up a massive break from the massive second row Tom Murray. Beating three tackles on his way to the half way line, the big man then had the control to secure possession as he took contact on his own terms and presented well.
It was back to defensive duty soon after however, as Swaffham were tested thoroughly by the big pack of the home side.
Haverhill were unlucky not to score as they secured ball from their own lineout and put in a cross-field kick. Fortunately for the men of Swaffham, the ball bounced safely over the dead ball line.
The centre partnership of Barnard and J Taylor was once again working well in both defence and attack, but there was no opportunity for them to break with ball in hand, so they concentrated on bringing the oncoming attackers down.
The half-time whistle went and Swaffham gathered round coach Wassell pleased with the defensive effort they had put in during a taxing and draining first half.
J Palmer scored halfway into the second half as J Taylor took a clean catch covering in the full-back position. The pack was there in numbers to secure possession at the ruck, but captain J Chamberlain had seen a weakness to exploit and was hanging back. He burst rampantly onto the inside flick from Lines and hit through a hole between the fly half and the breakdown.
He, in turn, fed Lines as he was eventually tackled and Lines put Palmer clean away to score his first try in Swaffham colours. The missed conversion meant the score stayed at 19-0.
The next try came just five minutes later as the exciting backs once again showed their full potential. Good defence from Lines saw Bartlett in possession. He stepped his man to burst up the line while J Taylor was blazing a trail in his support and plucked Bartlett's pass at full tilt. He had the presence of mind to return the pass to Bartlett as he was confronted with the hard-hitting Haverhill full-back.
Bartlett returned the favour over the line for Taylor to score, 24-0. J Trett was brought on for experienced campaigner M James, S Wood freshened up the back row in place of the hard-working M Taylor, while fresh-legged Pete Sparks brought youthfulness and added pace to the back division.
The final score came as Wood burst from the back of a scrum. From the base of the subsequent ruck Palmer had the vision to break blind where he outpaced his opposite man and offloaded to J Taylor who touched down with five minutes to go for a memorable Swaffham away win, 29-0 the final score.
Thurlow Nunn MoM: Tom Murray.


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You've got to admit that gentleman displays a pretty deft touch with the ol' chainsaw.
It's not that I disagree with Seth Emerson placing John Theus on his most important list.
It's that I'm worried he's underrated Theus' importance at No. 8.
In reaction to yesterday's news about the new Big 12-SEC postseason game, Paul Myerberg indulges in some romantic thinking.
This is a crisis moment for college football. It's also a look-in-the-mirror moment for those who dictate the game's ebb and flow: either the power-brokers – a Mike Slive, a Jim Delany, a Larry Scott, a Bob Bowlsby – can cater to their constituents, like a politician aiming for reelection, or they can do what's best for the game itself.
What's best for college football is equality. Don't be scared of that word: it doesn't mean socialism, and it doesn't necessarily mean parity. It means that deserving teams get what they deserve; it means that regardless of the size of your stadium, your career winning percentage, your TV contract or the name on the front of your jersey, you get a seat at the table.
The new system, when in place two years down the road, should ensure that each of every program in the F.B.S. can play for the national championship. It must, for the sake of college football itself. Anything less would be a continuation of our current, flawed system.
First of all, there's a real danger of getting way ahead of ourselves with this. All I feel confident about saying right now is congratulations to the two conferences for pulling off a power play: the Big 12 nailed the ACC badly and Slive has himself a nice bargaining chip to toss in when Delany's constituents figure out what they really want besides Rose Bowl Forevah! Besides that, who knows. It's too early to call this one item a game-changer.
That all being said, in response to Myerberg's dream, sorry, not gonna happen. Or at least not in the way he envisions. There are too many wheels in motion, too many forces in play for a 120 or so-school FBS to survive. Things like increased scholarship payments, multi-year scholarships and the end of AQ status for the postseason each on their own may not seem like much, but together they all point towards a sea change in D-1.
A separation between the NCAA haves and have-nots is coming. The only question for some is on which side of the divide they're going to fall. Jim Delany has never been fond of sharing. It's ironic that the new postseason may turn out to be the vehicle that gets him his wish.
It's been rumored for a while that he would be leaving, but at least he's wound up reuniting with his former position coach.
That completes a pretty radical transformation of Georgia's S&C staff.
… All of the assistants working under second-year coordinator Joe Tereshinski have left in the offseason: Keith Gray to the Philadelphia Eagles, Thomas Brown (another former Georgia player) to a coaching job at UT-Chattanooga, and Rex Bradberry for a job with the U.S. Special Forces.
John Kasay Jr., who had served in a part-time role on the staff, has also left.
– John Thomas, ,who ran Joe Paterno's strength program at Penn State for two decades, was hired as associate director.
– Sherman Armstrong was hired as a speed coach.


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CANBERRA OBSERVED: The origins of Labor's visceral loathing of Abbott
EDITORIAL: Swan's budget surplus to depend on mining tax
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EAST TIMOR: Election swing against Gusmão government
HUMAN RIGHTS: Academics who rationalise post-natal murder
POPULATION: Seven billion reasons to celebrate
OPINION: America: Russia's Afghan catspaw
OPINION: School textbook misleads about Crusades
WEIMAR GERMANY: Why art flourished and democracy perished
DOCUMENTARY: Lifting the veil on the global sex industry
Nefarious: Merchant of Souls (96 minutes)
CINEMA: Nihilism filtered through teen angst
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BOOK REVIEW The great class divide in the United States
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WEIMAR GERMANY:
Why art flourished and democracy perished
by Jeffry Babb
News Weekly, March 31, 2012
Weimar Germany saw an intense flowering of almost every form of creativity, yet this vibrant culture ran head first into Nazi Germany, which set out to destroy it.
The Weimar Republic was born amid chaos in the provincial city of Weimar in 1919 and died largely unmourned when the Nazis seized power in 1933.
It gained a reputation for vacillation, incompetence and weakness in the face of oppression by the victors of the Great War. It was burdened with the taint of betrayal — that the brave soldiers at the front, who after all were still on French and Belgium soil at the end of the war — had been "stabbed in the back" by the civilian government. Amazingly, the reparations demanded from Germany under the Treaty of Versailles were only finally paid off in 2010.
Three invalids (c.1930),
by German artist Heinrich Hoerle (1895–1936).
Private collection,
courtesy of the National Gallery of Victoria.
At first instance, the Weimar Republic would seem to be an unpromising environment for creativity. The three years of hyperinflation between 1921 and 1924 bankrupted the middle class and instilled an enduring fear of inflation. Tales are told of currency speculators who would drink their winnings every night because by morning their speculative gains would be worthless. A loaf of bread that cost one mark in 1921 could be bought for "only" 100 million marks in 1924.
The streets were inhabited by impoverished veterans with horrific wounds and prostitutes who traded in the drug of loneliness. The Freikorps, a paramilitary militia formed of veterans that fought sometimes for the state and sometimes against it, dealt harshly with those with whom it was displeased.
Why then was the Weimar Republic so productive in ideas and art? Because its flowering, like a hothouse plant, was so intense and short-lived, it has often been overlooked in Anglophone countries.
Berlin has frequently been overshadowed by its continental rival, Paris. Paris had "the Lost Generation" — Ernest Hemingway, Gertrude Stein and other litterateurs drinking their books away. It had Jean-Paul Sartre, and the Cubists — Pablo Picasso and Georges Braque. But with the revival of Germany as Europe's cultural hub as well as its financier, many would argue that Paris's pre-eminent reputation as the "between the wars" cultural capital of Europe is a triumph of publicity over substance. Berlin was the centre, but new creative movements sprang up all over Germany.
The depth and influence of Weimar culture was on show in Sydney and Melbourne recently in one of the most engrossing exhibitions in recent years, entitled "The Mad Square: Modernity in German Art, 1910–37". Surprisingly, half the exhibits are from Australian collections.
Of the painting which lends it name to the exhibition, guest curator Jacqueline Stecker writes: "Painted during a period of intense political and intellectual polarisation, The Mad Square by Felix Nussbaum can be seen as a satirisation of the collapse of society during the years of the Weimar Republic and a forewarning of the cataclysm that was to ensue."
Among the artistic movements which flourished in the Weimar period were Expressionism, Dada, Constructivism and New Objectivity. Of all the artistic and creative movements that thrived in the Weimar period, the one that has had the most influence on everyday life is Bauhaus. Or, as Tom Wolfe put it, "From Bauhaus to Our House."
To understand the profound influence Bauhaus has had on architecture and design, you have only to look around you. Almost every postwar skyscraper you see in any city in Australia is pure Bauhaus. Almost every kitchen utensil you use is influenced by Bauhaus design principles. The ubiquitous steel tubing chairs are pure Bauhaus.
Bauhaus was essentially a design studio that worked from first principles. The founder, Walter Gropius, was an architect, but in the first instance Bauhaus did not teach architecture. Bauhaus was not always a winner. In fact, it inflicted some horrible buildings on the world, including what the Americans call "projects" that did so much to criminalise and pauperise the less well-off, particularly inner city African-Americans.
The whole Weimar creative enterprise was about modernism. Modernism came late to Germany. Under Chancellor Count Otto von Bismarck, the Germans gained pensions, but at the cost of their freedom. The first democratic ruler of Germany was Prince Max of Baden, whose short-lived government attempted unsuccessfully to save Germany from chaos after the fighting ceased in 1918.
The underlying theme of the modernist project — that humans are moral beings who have the power to create, improve and reshape their environment through experimentation, scientific knowledge and technology — had suffered a near fatal blow in the blood-soaked trenches, where science aided, rather than hindered, the slaughter.
The last blow for modernism was the Degenerate Art exhibition, held in Munich in 1937. Hitler's offensive against the art of the Weimar Republic was intended to show the public that art that wasn't Aryan was immoral and corrupt. Art was certainly intended to be revolutionary, as artists aimed to overthrow rather than enlighten. The interwar flowering of German art was dead.
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TRANSGENDER: one shade of grey, 353pp, $39.99
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FOREIGN AFFAIRS Johnson to take UK out of the EU on January 31
VICTORIAN POLITICS Andrews hacks away at another way of life and source of jobs
COVER STORY A myriad transformations effected by one birth
CANBERRA OBSERVED Labor must own up to why it took the thrashing it got
THE QUEEN V PELL: A blight on the whole of the criminal justice system
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COVER STORY Wildfires: Lessons from the past not yet learnt
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